[ { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/3ha89-ae705", "eprint_status": "archive", "datestamp": "2023-10-16 21:23:30", "lastmod": "2023-10-16 21:29:44", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Yoo-Jooheon", "name": { "family": "Yoo", "given": "Jooheon" }, "orcid": "0000-0002-3251-0924" }, { "id": "Mitman-Keefe", "name": { "family": "Mitman", "given": "Keefe" }, "orcid": "0000-0003-0276-3856" }, { "id": "Varma-Vijay", "name": { "family": "Varma", "given": "Vijay" }, "orcid": "0000-0002-9994-1761" }, { "id": "Boyle-Michael", "name": { "family": "Boyle", "given": "Michael" }, "orcid": "0000-0002-5075-5116" }, { "id": "Field-Scott-E", "name": { "family": "Field", "given": "Scott E." }, "orcid": "0000-0002-6037-3277" }, { "id": "Deppe-Nils", "name": { "family": "Deppe", "given": "Nils" }, "orcid": "0000-0003-4557-4115" }, { "id": "H\u00e9bert-Fran\u00e7ois", "name": { "family": "H\u00e9bert", "given": "Fran\u00e7ois" }, "orcid": "0000-0001-9009-6955" }, { "id": "Kidder-Lawrence-E", "name": { "family": "Kidder", "given": "Lawrence E." }, "orcid": "0000-0001-5392-7342" }, { "id": "Moxon-Jordan", "name": { "family": "Moxon", "given": "Jordan" }, "orcid": "0000-0001-9891-8677" }, { "id": "Pfeiffer-Harald-P", "name": { "family": "Pfeiffer", "given": "Harald P." }, "orcid": "0000-0001-9288-519X" }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." }, "orcid": "0000-0001-6656-9134" }, { "id": "Stein-Leo-C", "name": { "family": "Stein", "given": "Leo C." }, "orcid": "0000-0001-7559-9597" }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" }, { "id": "Throwe-William", "name": { "family": "Throwe", "given": "William" }, "orcid": "0000-0001-5059-4378" }, { "id": "Vu-Nils-L", "name": { "family": "Vu", "given": "Nils L." }, "orcid": "0000-0002-5767-3949" } ] }, "title": "Numerical relativity surrogate model with memory effects and post-Newtonian hybridization", "ispublished": "pub", "full_text_status": "public", "note": "
\u00a9 2023 American Physical Society.
\n\nThis work was supported in part by the Sherman Fairchild Foundation and by NSF Grants No. PHY-2011961, No. PHY-2011968, and No. OAC-2209655 at Caltech, and NSF Grants No. PHY-2207342 and No. OAC-2209655 at Cornell. spectre uses charm++/converse [124], which was developed by the Parallel Programming Laboratory in the Department of Computer Science at the University of Illinois at Urbana-Champaign. V.\u2009V. acknowledges support from the European Union's Horizon 2020 research and innovation program under the Marie Sk\u0142odowska-Curie Grant agreement No. 896869. L.\u2009C.\u2009S. was partially supported by NSF CAREER Award PHY-2047382. S.\u2009E.\u2009F acknowledges partial support from NSF Grant PHY-2110496 and by UMass Dartmouth's Marine and Undersea Technology (MUST) Research Program funded by the Office of Naval Research (ONR) under Grant No. N00014-23-1\u20132141. This material is based upon work supported by NSF's LIGO Laboratory which is a major facility fully funded by the NSF. This project made use of python libraries including scipy [125] and numpy [126], and the figures were produced using matplotlib [127] and seaborn [128].
", "abstract": "Numerical relativity simulations provide the most precise templates for the gravitational waves produced by binary black hole mergers. However, many of these simulations use an incomplete waveform extraction technique\u2014extrapolation\u2014that fails to capture important physics, such as gravitational memory effects. Cauchy-characteristic evolution (CCE), by contrast, is a much more physically accurate extraction procedure that fully evolves Einstein's equations to future null infinity and accurately captures the expected physics. In this work, we present a new surrogate model, NRHybSur3dq8_CCE, built from CCE waveforms that have been mapped to the post-Newtonian (PN) BMS frame and then hybridized with PN and effective one-body (EOB) waveforms. This model is trained on 102 waveforms with mass ratios q \u2264 8 and aligned spins \u03c7_(1z),\u03c7_(2z) \u2208 [\u22120.8,0.8]. The model spans the entire LIGO-Virgo-KAGRA (LVK) frequency band (with flow = 20\u2009\u2009Hz) for total masses M \u2273 2.25 M_\u2299 and includes the \u2113 \u2264 4 and (\u2113,m)=(5,5) spin-weight \u22122 spherical harmonic modes, but not the (3, 1), (4, 2) or (4, 1) modes. We find that NRHybSur3dq8_CCE can accurately reproduce the training waveforms with mismatches \u22722 \u00d7 10\u207b\u2074 for total masses 2.2 5M_\u2299 \u2264 M \u2264 300 M_\u2299 and can, for a modest degree of extrapolation, capably model outside of its training region. Most importantly, unlike previous waveform models, the new surrogate model successfully captures memory effects.
", "date": "2023-09-15", "date_type": "published", "publication": "Physical Review D", "volume": "108", "number": "6", "publisher": "American Physical Society", "pagerange": "064027", "issn": "2470-0010", "official_url": "https://authors.library.caltech.edu/records/3ha89-ae705", "funders": { "items": [ {}, { "grant_number": "PHY-2011961" }, { "grant_number": "PHY-2011968" }, { "grant_number": "OAC-2209655" }, { "grant_number": "PHY-2207342" }, { "grant_number": "896869" }, { "grant_number": "PHY-2047382" }, { "grant_number": "PHY-2110496" }, { "grant_number": "N00014-23-1\u20132141" } ] }, "local_group": { "items": [ { "id": "TAPIR" }, { "id": "Walter-Burke-Institute-for-Theoretical-Physics" }, { "id": "LIGO" } ] }, "doi": "10.1103/physrevd.108.064027", "primary_object": { "basename": "PhysRevD.108.064027.pdf", "url": "https://authors.library.caltech.edu/records/3ha89-ae705/files/PhysRevD.108.064027.pdf" }, "resource_type": "article", "pub_year": "2023", "author_list": "Yoo, Jooheon; Mitman, Keefe; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/24v0s-kh838", "eprint_id": 121122, "eprint_status": "archive", "datestamp": "2023-08-20 16:43:21", "lastmod": "2023-10-23 15:38:55", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Moxon-Jordan", "name": { "family": "Moxon", "given": "Jordan" }, "orcid": "0000-0001-9891-8677" }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." }, "orcid": "0000-0001-6656-9134" }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" }, { "id": "Deppe-Nils", "name": { "family": "Deppe", "given": "Nils" }, "orcid": "0000-0003-4557-4115" }, { "id": "Vu-Nils-L", "name": { "family": "Vu", "given": "Nils" }, "orcid": "0000-0002-5767-3949" }, { "id": "H\u00e9bert-Fran\u00e7ois", "name": { "family": "H\u00e9bert", "given": "Francois" }, "orcid": "0000-0001-9009-6955" }, { "id": "Kidder-Lawrence-E", "name": { "family": "Kidder", "given": "Lawrence E." }, "orcid": "0000-0001-5392-7342" }, { "id": "Throwe-William", "name": { "family": "Throwe", "given": "William" }, "orcid": "0000-0001-5059-4378" } ] }, "title": "SpECTRE Cauchy-characteristic evolution system for rapid, precise waveform extraction", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2023 American Physical Society. \n\nWe thank Kevin Barkett, Keefe Mitman, and Sizheng Ma for valuable discussions and suggestions regarding this project. This work was supported in part by the Sherman Fairchild Foundation and by National Science Foundation (NSF) Grants No. PHY-2011961, No. PHY-2011968, and No. OAC-1931266 at Caltech and NSF Grants No. PHY-1912081 and No. OAC-1931280 at Cornell.\n\nPublished - PhysRevD.107.064013.pdf
", "abstract": "We give full details regarding the new Cauchy-characteristic evolution (CCE) system in spectre. The implementation is built to provide streamlined flexibility for either extracting waveforms during the process of a spectre binary compact object simulation or as a stand-alone module for extracting waveforms from worldtube data provided by another code base. Using our recently presented improved analytic formulation, the CCE system is free of pure-gauge logarithms that would spoil the spectral convergence of the scheme. It gracefully extracts all five Weyl scalars, in addition to the news and the strain. The spectre CCE system makes significant improvements on previous implementations in modularity, ease of use, and speed of computation.", "date": "2023-03-15", "date_type": "published", "publication": "Physical Review D", "volume": "107", "number": "6", "publisher": "American Physical Society", "pagerange": "Art. No. 064013", "id_number": "CaltechAUTHORS:20230420-698969800.11", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230420-698969800.11", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Sherman Fairchild Foundation" }, { "agency": "NSF", "grant_number": "PHY-2011961" }, { "agency": "NSF", "grant_number": "PHY-2011968" }, { "agency": "NSF", "grant_number": "OAC-1931266" }, { "agency": "NSF", "grant_number": "PHY-1912081" }, { "agency": "NSF", "grant_number": "OAC-1931280" } ] }, "local_group": { "items": [ { "id": "TAPIR" }, { "id": "Walter-Burke-Institute-for-Theoretical-Physics" } ] }, "doi": "10.1103/physrevd.107.064013", "primary_object": { "basename": "PhysRevD.107.064013.pdf", "url": "https://authors.library.caltech.edu/records/24v0s-kh838/files/PhysRevD.107.064013.pdf" }, "resource_type": "article", "pub_year": "2023", "author_list": "Moxon, Jordan; Scheel, Mark A.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/fd4bp-3t733", "eprint_id": 119484, "eprint_status": "archive", "datestamp": "2023-08-22 19:05:26", "lastmod": "2023-10-23 20:20:28", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Mitman-Keefe", "name": { "family": "Mitman", "given": "Keefe" }, "orcid": "0000-0003-0276-3856" }, { "id": "Lagos-Macarena", "name": { "family": "Lagos", "given": "Macarena" }, "orcid": "0000-0003-0234-9970" }, { "id": "Stein-Leo-C", "name": { "family": "Stein", "given": "Leo C." }, "orcid": "0000-0001-7559-9597" }, { "id": "Ma-Sizheng", "name": { "family": "Ma", "given": "Sizheng" }, "orcid": "0000-0002-4645-453X" }, { "id": "Hui-Lam", "name": { "family": "Hui", "given": "Lam" } }, { "id": "Chen-Yanbei", "name": { "family": "Chen", "given": "Yanbei" }, "orcid": "0000-0002-9730-9463" }, { "id": "Deppe-Nils", "name": { "family": "Deppe", "given": "Nils" }, "orcid": "0000-0003-4557-4115" }, { "id": "H\u00e9bert-Fran\u00e7ois", "name": { "family": "H\u00e9bert", "given": "Fran\u00e7ois" }, "orcid": "0000-0001-9009-6955" }, { "id": "Kidder-Lawrence-E", "name": { "family": "Kidder", "given": "Lawrence E." }, "orcid": "0000-0001-5392-7342" }, { "id": "Moxon-Jordan", "name": { "family": "Moxon", "given": "Jordan" }, "orcid": "0000-0001-9891-8677" }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." }, "orcid": "0000-0001-6656-9134" }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" }, { "id": "Throwe-William", "name": { "family": "Throwe", "given": "William" }, "orcid": "0000-0001-5059-4378" }, { "id": "Vu-Nils-L", "name": { "family": "Vu", "given": "Nils L." }, "orcid": "0000-0002-5767-3949" } ] }, "title": "Nonlinearities in Black Hole Ringdowns", "ispublished": "pub", "full_text_status": "public", "keywords": "General Physics and Astronomy", "note": "We thank Max Isi and the Flatiron Institute for fostering discourse, and Vishal Baibhav, Emanuele Berti, Mark Cheung, Matt Giesler, Scott Hughes, and Max Isi for valuable conversations. Computations for this work were performed with the Wheeler cluster at Caltech. This work was supported in part by the Sherman Fairchild Foundation and by NSF Grants No. PHY-2011961, No. PHY-2011968, and No. OAC-1931266 at Caltech, as well as NSF Grants No. PHY-1912081, No. PHY-2207342, and No. OAC-1931280 at Cornell. The work of L.\u2009C.\u2009S. was partially supported by NSF CAREER Grant No. PHY-2047382. M.\u2009L. was funded by the Innovative Theoretical Cosmology Fellowship at Columbia University. L.\u2009H. was funded by the DOE DE-SC0011941 and a Simons Fellowship in Theoretical Physics. M.\u2009L. and L.\u2009C.\u2009S. thank the Benasque Science Center and the organizers of the 2022 workshop \"New frontiers in strong gravity,\" where some of this work was performed; and M.\u2009L. acknowledges NSF Grant No. PHY-1759835 for supporting travel to this workshop.", "abstract": "The gravitational wave strain emitted by a perturbed black hole (BH) ringing down is typically modeled analytically using first-order BH perturbation theory. In this Letter we show that second-order effects are necessary for modeling ringdowns from BH merger simulations. Focusing on the strain's (\u2113,m)=(4,4) angular harmonic, we show the presence of a quadratic effect across a range of binary BH mass ratios that agrees with theoretical expectations. We find that the quadratic (4,4) mode amplitude exhibits quadratic scaling with the fundamental (2,2) mode -- its parent mode. The nonlinear mode's amplitude is comparable to or even larger than that of the linear (4,4) modes. Therefore correctly modeling ringdown -- improving mismatches by an order of magnitude -- requires the inclusion of nonlinear effects.", "date": "2023-02-24", "date_type": "published", "publication": "Physical Review Letters", "volume": "130", "number": "8", "publisher": "American Physical Society", "pagerange": "Art. No. 081402", "id_number": "CaltechAUTHORS:20230223-726432000.5", "issn": "0031-9007", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230223-726432000.5", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Sherman Fairchild Foundation" }, { "agency": "NSF", "grant_number": "PHY-2011961" }, { "agency": "NSF", "grant_number": "PHY-2011968" }, { "agency": "NSF", "grant_number": "OAC-1931266" }, { "agency": "NSF", "grant_number": "PHY-1912081" }, { "agency": "NSF", "grant_number": "PHY-2207342" }, { "agency": "NSF", "grant_number": "OAC-1931280" }, { "agency": "NSF", "grant_number": "PHY-2047382" }, { "agency": "Columbia University" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-SC0011941" }, { "agency": "Simons Foundation" }, { "agency": "NSF", "grant_number": "PHY-1759835" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" }, { "id": "TAPIR" } ] }, "doi": "10.1103/physrevlett.130.081402", "resource_type": "article", "pub_year": "2023", "author_list": "Mitman, Keefe; Lagos, Macarena; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/jfasc-6za46", "eprint_id": 119472, "eprint_status": "archive", "datestamp": "2023-08-20 08:26:44", "lastmod": "2023-10-23 15:28:42", "type": "monograph", "metadata_visibility": "show", "creators": { "items": [ { "id": "Mitman-Keefe", "name": { "family": "Mitman", "given": "Keefe" }, "orcid": "0000-0003-0276-3856" }, { "id": "Lagos-Macarena", "name": { "family": "Lagos", "given": "Macarena" }, "orcid": "0000-0003-0234-9970" }, { "id": "Stein-Leo-C", "name": { "family": "Stein", "given": "Leo C." }, "orcid": "0000-0001-7559-9597" }, { "id": "Ma-Sizheng", "name": { "family": "Ma", "given": "Sizheng" }, "orcid": "0000-0002-4645-453X" }, { "id": "Hui-Lam", "name": { "family": "Hui", "given": "Lam" } }, { "id": "Chen-Yanbei", "name": { "family": "Chen", "given": "Yanbei" }, "orcid": "0000-0002-9730-9463" }, { "id": "Deppe-Nils", "name": { "family": "Deppe", "given": "Nils" }, "orcid": "0000-0003-4557-4115" }, { "id": "H\u00e9bert-Fran\u00e7ois", "name": { "family": "H\u00e9bert", "given": "Fran\u00e7ois" }, "orcid": "0000-0001-9009-6955" }, { "id": "Kidder-Lawrence-E", "name": { "family": "Kidder", "given": "Lawrence E." }, "orcid": "0000-0001-5392-7342" }, { "id": "Moxon-Jordan", "name": { "family": "Moxon", "given": "Jordan" }, "orcid": "0000-0001-9891-8677" }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." }, "orcid": "0000-0001-6656-9134" }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" }, { "id": "Throwe-William", "name": { "family": "Throwe", "given": "William" }, "orcid": "0000-0001-5059-4378" }, { "id": "Vu-Nils-L", "name": { "family": "Vu", "given": "Nils L." }, "orcid": "0000-0002-5767-3949" } ] }, "title": "Nonlinearities in black hole ringdowns", "ispublished": "unpub", "full_text_status": "public", "note": "Attribution 4.0 International (CC BY 4.0) \n\nWe thank Max Isi and the Flatiron Institute for fostering discourse, and Vishal Baibhav, Emanuele Berti, Mark Cheung, Matt Giesler, Scott Hughes, and Max Isi for valuable conversations. Computations for this work were performed with the Wheeler cluster at Caltech. This work was supported in part by the Sherman Fairchild Foundation and by NSF Grants No. PHY-2011961, No. PHY-2011968, and No. OAC-1931266 at Caltech, as well as NSF Grants No. PHY-1912081, No. PHY-2207342, and No. OAC-1931280 at Cornell. The work of L.C.S. was partially supported by NSF CAREER Award PHY-2047382. M.L. was funded by the Innovative Theoretical Cosmology Fellowship at Columbia University. L.H. was funded by the DOE DE-SC0011941 and a Simons Fellowship in Theoretical Physics. M.L. and L.C.S. thank the Benasque Science Center and the organizers of the 2022 workshop \"New frontiers in strong gravity,\" where some of this work was performed; and M.L. acknowledges NSF Grant No. PHY-1759835 for supporting travel to this workshop.\n\nSubmitted - 2208.07380.pdf
", "abstract": "The gravitational wave strain emitted by a perturbed black hole (BH) ringing down is typically modeled analytically using first-order BH perturbation theory. In this Letter we show that second-order effects are necessary for modeling ringdowns from BH merger simulations. Focusing on the strain's (\u2113,m)=(4,4) angular harmonic, we show the presence of a quadratic effect across a range of binary BH mass ratios that agrees with theoretical expectations. We find that the quadratic (4,4) mode amplitude exhibits quadratic scaling with the fundamental (2,2) mode -- its parent mode. The nonlinear mode's amplitude is comparable to or even larger than that of the linear (4,4) modes. Therefore correctly modeling ringdown -- improving mismatches by an order of magnitude -- requires the inclusion of nonlinear effects.", "date": "2023-02-22", "date_type": "published", "publisher": "arXiv", "id_number": "CaltechAUTHORS:20230222-200216505", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230222-200216505", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Sherman Fairchild Foundation" }, { "agency": "NSF", "grant_number": "PHY-2011961" }, { "agency": "NSF", "grant_number": "PHY-2011968" }, { "agency": "NSF", "grant_number": "OAC-1931266" }, { "agency": "NSF", "grant_number": "PHY-1912081" }, { "agency": "NSF", "grant_number": "PHY-2207342" }, { "agency": "NSF", "grant_number": "OAC-1931280" }, { "agency": "NSF", "grant_number": "PHY-2047382" }, { "agency": "Columbia University" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-SC0011941" }, { "agency": "Simons Foundation" }, { "agency": "NSF", "grant_number": "PHY-1759835" } ] }, "local_group": { "items": [ { "id": "TAPIR" }, { "id": "Astronomy-Department" } ] }, "doi": "10.48550/arXiv.2208.07380", "primary_object": { "basename": "2208.07380.pdf", "url": "https://authors.library.caltech.edu/records/jfasc-6za46/files/2208.07380.pdf" }, "resource_type": "monograph", "pub_year": "2023", "author_list": "Mitman, Keefe; Lagos, Macarena; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/129ej-59f55", "eprint_id": 119608, "eprint_status": "archive", "datestamp": "2023-08-20 09:01:17", "lastmod": "2023-10-25 15:59:55", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bonilla-Gabriel-S", "name": { "family": "Bonilla", "given": "Gabriel S." }, "orcid": "0000-0003-4502-528X" }, { "id": "Kumar-Prayush", "name": { "family": "Kumar", "given": "Prayush" }, "orcid": "0000-0001-5523-4603" }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Modeling compact binary merger waveforms beyond general relativity", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2023 American Physical Society. \n\nWe thank \u00c9amonn O'Shea and Masha Okounkova for useful discussions, and Shasvath Kapadia, Daiki Watarai, Swati Singh, and Srashti Goyal for their careful reading of the manuscript. This work was supported in part by the Sherman Fairchild Foundation, and by NSF Grant No. PHY-1912081 at Cornell. This work was also supported in part by NSF Grants No. PHY-1654359 and No. PHY-2208014, by the Dan Black Family Trust, and by Nicholas and Lee Begovich at Cal State Fullerton. P.\u2009K. acknowledges support of the Department of Atomic Energy, Government of India, under project no. RTI4001; and by the Ashok and Gita Vaish Early Career Faculty Fellowship at the International Centre for Theoretical Sciences. The authors are grateful for computational resources provided by the LIGO Laboratory and supported by National Science Foundation Grants No. PHY-0757058 and No. PHY-0823459.\n\nPublished - PhysRevD.107.024015.pdf
", "abstract": "The parametrized post-Einsteinian framework modifies inspiral waveform models to incorporate effects beyond general relativity (GR). We extend the existing model into the merger-ringdown regime. The modification introduced here adds a single degree of freedom that corresponds to a change in the binary coalescence time. Other merger properties remain as predicted by GR. We discuss parameter estimation with this model, and how it can be used to extract information from beyond-GR waveforms.", "date": "2023-01-15", "date_type": "published", "publication": "Physical Review D", "volume": "107", "number": "2", "publisher": "American Physical Society", "pagerange": "Art. No. 024015", "id_number": "CaltechAUTHORS:20230301-701033500.8", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230301-701033500.8", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Sherman Fairchild Foundation" }, { "agency": "NSF", "grant_number": "PHY-1912081" }, { "agency": "NSF", "grant_number": "PHY-1654359" }, { "agency": "NSF", "grant_number": "PHY-2208014" }, { "agency": "Dan Black Family Trust" }, { "agency": "California State University, Fullerton" }, { "agency": "Department of Atomic Energy (India)", "grant_number": "RTI4001" }, { "agency": "International Centre for Theoretical Sciences" }, { "agency": "NSF", "grant_number": "PHY-0823459" }, { "agency": "NSF", "grant_number": "PHY-0757058" }, { "agency": "LIGO Laboratory" } ] }, "local_group": { "items": [ { "id": "TAPIR" }, { "id": "Walter-Burke-Institute-for-Theoretical-Physics" } ] }, "doi": "10.1103/physrevd.107.024015", "primary_object": { "basename": "PhysRevD.107.024015.pdf", "url": "https://authors.library.caltech.edu/records/129ej-59f55/files/PhysRevD.107.024015.pdf" }, "resource_type": "article", "pub_year": "2023", "author_list": "Bonilla, Gabriel S.; Kumar, Prayush; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/x4c6m-9yg33", "eprint_id": 119172, "eprint_status": "archive", "datestamp": "2023-08-20 08:55:15", "lastmod": "2023-10-23 15:30:12", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Chen-Yitian", "name": { "family": "Chen", "given": "Yitian" }, "orcid": "0000-0002-8664-9702" }, { "id": "Kumar-Prayush", "name": { "family": "Kumar", "given": "Prayush" }, "orcid": "0000-0001-5523-4603" }, { "id": "Khera-Neev", "name": { "family": "Khera", "given": "Neev" }, "orcid": "0000-0003-3515-2859" }, { "id": "Deppe-Nils", "name": { "family": "Deppe", "given": "Nils" }, "orcid": "0000-0003-4557-4115" }, { "id": "Dhani-Arnab", "name": { "family": "Dhani", "given": "Arnab" }, "orcid": "0000-0001-9930-9101" }, { "id": "Boyle-Michael", "name": { "family": "Boyle", "given": "Michael" }, "orcid": "0000-0002-5075-5116" }, { "id": "Giesler-Matthew-D", "name": { "family": "Giesler", "given": "Matthew" }, "orcid": "0000-0003-2300-893X" }, { "id": "Kidder-Lawrence-E", "name": { "family": "Kidder", "given": "Lawrence E." }, "orcid": "0000-0001-5392-7342" }, { "id": "Pfeiffer-Harald-P", "name": { "family": "Pfeiffer", "given": "Harald P." }, "orcid": "0000-0001-9288-519X" }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." }, "orcid": "0000-0001-6656-9134" }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Multipole moments on the common horizon in a binary-black-hole simulation", "ispublished": "pub", "full_text_status": "public", "note": "We thank Abhay Ashtekar, Bangalore Sathyaprakash, Ssohrab Borhanian, Leo Stein, and Robert Owen for useful discussions. Computations for this work were performed with the Wheeler cluster at Caltech and the Bridges system (and XSEDE) at the Pittsburgh Supercomputing Center (PSC). This work was supported in part by the Sherman Fairchild Foundation and by NSF Grants No. PHY-2011961, No. PHY-2011968, and No. OAC-1931266 at Caltech, as well as NSF Grants No. PHY-1912081, No. OAC-1931280, and No. PHY-2209655 at Cornell. This work was also supported by NSF Grant No. PHY-1806356, No. PHY-2012083, the Eberly Chair funds of Penn State University, and the Mebus Fellowship to N.\u2009K. P.\u2009K. acknowledges support of the Department of Atomic Energy, Government of India, under Project No. RTI4001, and of the Ashok and Gita Vaish Early Career Faculty Fellowship at the International Centre for Theoretical Sciences.", "abstract": "We construct the covariantly defined multipole moments on the common horizon of an equal-mass, nonspinning, quasicircular binary-black-hole system. We see a strong correlation between these multipole moments and the gravitational waveform. We find that the multipole moments are well described by the fundamental quasinormal modes at sufficiently late times. For each nonzero multipole moment with \u2113 \u2264 6, at least two fundamental quasinormal modes of different \u2113 are detectable in the best model. These models provide faithful estimates of the true mass and spin of the remnant black hole. We also show that by including overtones, the \u2113 = m = 2 mass multipole moment admits an excellent quasinormal-mode description at all times after the merger. This demonstrates the perhaps surprising power of perturbation theory near the merger.", "date": "2022-12-29", "date_type": "published", "publication": "Physical Review D", "volume": "106", "number": "12", "publisher": "American Physical Society", "id_number": "CaltechAUTHORS:20230209-988069100.5", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230209-988069100.5", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Sherman Fairchild Foundation" }, { "agency": "NSF", "grant_number": "PHY-2011961" }, { "agency": "NSF", "grant_number": "PHY-2011968" }, { "agency": "NSF", "grant_number": "OAC-1931266" }, { "agency": "NSF", "grant_number": "PHY-1912081" }, { "agency": "NSF", "grant_number": "OAC-1931280" }, { "agency": "NSF", "grant_number": "PHY-2209655" }, { "agency": "NSF", "grant_number": "PHY-1806356" }, { "agency": "NSF", "grant_number": "PHY-2012083" }, { "agency": "Pennsylvania State University" }, { "agency": "Department of Atomic Energy (India)", "grant_number": "RTI4001" }, { "agency": "International Centre for Theoretical Sciences" } ] }, "local_group": { "items": [ { "id": "TAPIR" } ] }, "doi": "10.1103/physrevd.106.124045", "resource_type": "article", "pub_year": "2022", "author_list": "Chen, Yitian; Kumar, Prayush; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/pxwg5-60623", "eprint_id": 116863, "eprint_status": "archive", "datestamp": "2023-08-22 17:54:42", "lastmod": "2023-10-24 21:10:19", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Deppe-Nils", "name": { "family": "Deppe", "given": "Nils" }, "orcid": "0000-0003-4557-4115" }, { "id": "H\u00e9bert-Fran\u00e7ois", "name": { "family": "H\u00e9bert", "given": "Fran\u00e7ois" }, "orcid": "0000-0001-9009-6955" }, { "id": "Kidder-Lawrence-E", "name": { "family": "Kidder", "given": "Lawrence E." }, "orcid": "0000-0001-5392-7342" }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "A high-order shock capturing discontinuous Galerkin-finite difference hybrid method for GRMHD", "ispublished": "pub", "full_text_status": "public", "keywords": "Physics and Astronomy (miscellaneous)", "note": "Charm++/Converse [85] was developed by the Parallel Programming Laboratory in the Department of Computer Science at the University of Illinois at Urbana-Champaign. The figures in this article were produced with matplotlib [86, 87], TikZ [88] and ParaView [89, 90]. Computations were performed with the Wheeler cluster at Caltech. This work was supported in part by the Sherman Fairchild Foundation and by NSF Grant Nos. PHY-2011961, PHY-2011968, and OAC-1931266 at Caltech, and NSF Grant Nos. PHY-1912081 and OAC-1931280 at Cornell.", "abstract": "We present a discontinuous Galerkin (DG)\u2013finite difference (FD) hybrid scheme that allows high-order shock capturing with the DG method for general relativistic magnetohydrodynamics. The hybrid method is conceptually quite simple. An unlimited DG candidate solution is computed for the next time step. If the candidate solution is inadmissible, the time step is retaken using robust FD methods. Because of its a posteriori nature, the hybrid scheme inherits the best properties of both methods. It is high-order with exponential convergence in smooth regions, while robustly handling discontinuities. We give a detailed description of how we transfer the solution between the DG and FD solvers, and the troubled-cell indicators necessary to robustly handle slow-moving discontinuities and simulate magnetized neutron stars. We demonstrate the efficacy of the proposed method using a suite of standard and very challenging 1D, 2D, and 3D relativistic magnetohydrodynamics test problems. The hybrid scheme is designed from the ground up to efficiently simulate astrophysical problems such as the inspiral, coalescence, and merger of two neutron stars.", "date": "2022-10-06", "date_type": "published", "publication": "Classical and Quantum Gravity", "volume": "39", "number": "19", "publisher": "Institute of Physics", "pagerange": "Art. No. 195001", "id_number": "CaltechAUTHORS:20220909-232652000", "issn": "0264-9381", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220909-232652000", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY-2011961" }, { "agency": "Sherman Fairchild Foundation" }, { "agency": "NSF", "grant_number": "PHY-2011968" }, { "agency": "NSF", "grant_number": "OAC-1931266" }, { "agency": "NSF", "grant_number": "PHY-1912081" }, { "agency": "NSF", "grant_number": "OAC-1931280" } ] }, "local_group": { "items": [ { "id": "TAPIR" } ] }, "doi": "10.1088/1361-6382/ac8864", "resource_type": "article", "pub_year": "2022", "author_list": "Deppe, Nils; H\u00e9bert, Fran\u00e7ois; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/qeq0t-zyc59", "eprint_id": 115633, "eprint_status": "archive", "datestamp": "2023-08-20 07:58:39", "lastmod": "2023-10-23 15:23:08", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Deppe-Nils", "name": { "family": "Deppe", "given": "Nils" }, "orcid": "0000-0003-4557-4115" }, { "id": "H\u00e9bert-Fran\u00e7ois", "name": { "family": "H\u00e9bert", "given": "Fran\u00e7ois" }, "orcid": "0000-0001-9009-6955" }, { "name": { "family": "Kidder", "given": "Lawrence E." }, "orcid": "0000-0001-5392-7342" }, { "name": { "family": "Throwe", "given": "William" }, "orcid": "0000-0001-5059-4378" }, { "name": { "family": "Anantpurkar", "given": "Isha" } }, { "name": { "family": "Armaza", "given": "Crist\u00f3bal" } }, { "name": { "family": "Bonilla", "given": "Gabriel S." }, "orcid": "0000-0003-4502-528X" }, { "name": { "family": "Boyle", "given": "Michael" }, "orcid": "0000-0002-5075-5116" }, { "id": "Chaudhary-Himanshu", "name": { "family": "Chaudhary", "given": "Himanshu" }, "orcid": "0000-0002-4101-0534" }, { "name": { "family": "Duez", "given": "Matthew D." }, "orcid": "0000-0002-0050-1783" }, { "name": { "family": "Vu", "given": "Nils L." }, "orcid": "0000-0002-5767-3949" }, { "name": { "family": "Foucart", "given": "Fran\u00e7ois" }, "orcid": "0000-0003-4617-4738" }, { "name": { "family": "Giesler", "given": "Matthew" }, "orcid": "0000-0003-2300-893X" }, { "name": { "family": "Guo", "given": "Jason S." }, "orcid": "0000-0002-5196-4104" }, { "id": "Kim-Yoonsoo", "name": { "family": "Kim", "given": "Yoonsoo" } }, { "name": { "family": "Kumar", "given": "Prayush" } }, { "id": "Legred-Isaac", "name": { "family": "Legred", "given": "Isaac" }, "orcid": "0000-0002-9523-9617" }, { "id": "Li-Dongjun", "name": { "family": "Li", "given": "Dongjun" } }, { "name": { "family": "Lovelace", "given": "Geoffrey" }, "orcid": "0000-0002-7084-1070" }, { "id": "Ma-Sizheng", "name": { "family": "Ma", "given": "Sizheng" }, "orcid": "0000-0002-4645-453X" }, { "name": { "family": "Macedo", "given": "Alexandra" } }, { "name": { "family": "Melchor", "given": "Denyz" } }, { "name": { "family": "Morales", "given": "Marlo" } }, { "id": "Moxon-Jordan", "name": { "family": "Moxon", "given": "Jordan" }, "orcid": "0000-0001-9891-8677" }, { "id": "Nelli-Kyle-C", "name": { "family": "Nelli", "given": "Kyle C." }, "orcid": "0000-0003-2426-8768" }, { "name": { "family": "O'Shea", "given": "Eamonn" }, "orcid": "0000-0002-0230-9533" }, { "name": { "family": "Pfeiffer", "given": "Harald P." }, "orcid": "0000-0001-9288-519X" }, { "name": { "family": "Ramirez", "given": "Teresita" } }, { "name": { "family": "R\u00fcter", "given": "Hannes R." } }, { "name": { "family": "Sanchez", "given": "Jennifer" } }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." }, "orcid": "0000-0001-6656-9134" }, { "name": { "family": "Thomas", "given": "Sierra" } }, { "name": { "family": "Vieira", "given": "Daniel" }, "orcid": "0000-0001-8019-0390" }, { "name": { "family": "Wittek", "given": "Nikolas A." }, "orcid": "0000-0001-8575-5450" }, { "name": { "family": "Wlodarczyk", "given": "Tom" } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Simulating magnetized neutron stars with discontinuous Galerkin methods", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2022 American Physical Society. \n\n(Received 29 September 2021; revised 6 May 2022; accepted 1 June 2022; published 27 June 2022) \n\nCharm++/Converse [83] was developed by the Parallel Programming Laboratory in the Department of Computer Science at the University of Illinois at Urbana-Champaign. The figures in this article were produced with matplotlib [84,85], tikz [86] and paraview [87,88]. Computations were performed with the Wheeler cluster at Caltech. This work was supported in part by the Sherman Fairchild Foundation and by NSF Grants No. PHY-2011961, No. PHY-2011968, and No. OAC-1931266 at Caltech, and NSF Grants No. PHY- 1912081 and No. OAC-1931280 at Cornell. P.\u2009K. acknowledges support of the Department of Atomic Energy, Government of India, under Project No. RTI4001, and by the Ashok and Gita Vaish Early Career Faculty Fellowship at the International Centre for Theoretical Sciences. M.\u2009D. acknowledges support from the NSF through Grant No. PHY-2110287. F.\u2009F. acknowledges support from the DOE through Grant No. DE-SC0020435, from NASA through Grant No. 80NSSC18K0565 and from the NSF through Grant No. PHY-1806278. G.\u2009L. is pleased to acknowledge support from the NSF through Grants No. PHY-1654359 and No. AST-1559694 and from Nicholas and Lee Begovich and the Dan Black Family Trust. H.\u2009R.\u2009R. acknowledges support from the Funda\u00e7\u00e3o para a Ci\u00eancia e Tecnologia (FCT) within the Projects No. UID/04564/2021, No. UIDB/04564/2020, No. UIDP/04564/2020 and No. EXPL/FIS-AST/0735/2021.\n\nPublished - PhysRevD.105.123031.pdf
Accepted Version - 2109.12033.pdf
", "abstract": "Discontinuous Galerkin methods are popular because they can achieve high order where the solution is smooth, because they can capture shocks while needing only nearest-neighbor communication, and because they are relatively easy to formulate on complex meshes. We perform a detailed comparison of various limiting strategies presented in the literature applied to the equations of general relativistic magnetohydrodynamics. We compare the standard minmod/\u039b\u03a0\u1d3a limiter, the hierarchical limiter of Krivodonova, the simple WENO limiter, the HWENO limiter, and a discontinuous Galerkin-finite-difference hybrid method. The ultimate goal is to understand what limiting strategies are able to robustly simulate magnetized Tolman-Oppenheimer-Volkoff stars without any fine-tuning of parameters. Among the limiters explored here, the only limiting strategy we can endorse is a discontinuous Galerkin-finite-difference hybrid method.", "date": "2022-06-15", "date_type": "published", "publication": "Physical Review D", "volume": "105", "number": "12", "publisher": "American Physical Society", "pagerange": "Art. No. 123031", "id_number": "CaltechAUTHORS:20220715-332513000", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220715-332513000", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Sherman Fairchild Foundation" }, { "agency": "NSF", "grant_number": "PHY-2011961" }, { "agency": "NSF", "grant_number": "PHY-2011968" }, { "agency": "NSF", "grant_number": "OAC-1931266" }, { "agency": "NSF", "grant_number": "PHY-1912081" }, { "agency": "NSF", "grant_number": "OAC-1931280" }, { "agency": "Department of Atomic Energy (India)", "grant_number": "RTI4001" }, { "agency": "International Centre for Theoretical Sciences" }, { "agency": "NSF", "grant_number": "PHY-2110287" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-SC0020435" }, { "agency": "NASA", "grant_number": "80NSSC18K0565" }, { "agency": "NSF", "grant_number": "PHY-1806278" }, { "agency": "NSF", "grant_number": "PHY-1654359" }, { "agency": "NSF", "grant_number": "AST-1559694" }, { "agency": "Nicholas and Lee Begovich" }, { "agency": "Dan Black Family Trust" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)", "grant_number": "UID/04564/2021" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)", "grant_number": "UIDB/04564/2020" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)", "grant_number": "UIDP/04564/2020" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)", "grant_number": "EXPL/FIS-AST/0735/2021" } ] }, "local_group": { "items": [ { "id": "TAPIR" } ] }, "doi": "10.1103/physrevd.105.123031", "primary_object": { "basename": "2109.12033.pdf", "url": "https://authors.library.caltech.edu/records/qeq0t-zyc59/files/2109.12033.pdf" }, "related_objects": [ { "basename": "PhysRevD.105.123031.pdf", "url": "https://authors.library.caltech.edu/records/qeq0t-zyc59/files/PhysRevD.105.123031.pdf" } ], "resource_type": "article", "pub_year": "2022", "author_list": "Deppe, Nils; H\u00e9bert, Fran\u00e7ois; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/hhpz3-00q98", "eprint_id": 114989, "eprint_status": "archive", "datestamp": "2023-08-20 07:42:11", "lastmod": "2023-10-23 15:16:39", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Maga\u00f1a-Zertuche-Lorena", "name": { "family": "Maga\u00f1a Zertuche", "given": "Lorena" }, "orcid": "0000-0003-1888-9904" }, { "id": "Mitman-Keefe", "name": { "family": "Mitman", "given": "Keefe" }, "orcid": "0000-0003-0276-3856" }, { "id": "Khera-Neev", "name": { "family": "Khera", "given": "Neev" }, "orcid": "0000-0003-3515-2859" }, { "id": "Stein-Leo-C", "name": { "family": "Stein", "given": "Leo C." }, "orcid": "0000-0001-7559-9597" }, { "id": "Boyle-Michael", "name": { "family": "Boyle", "given": "Michael" }, "orcid": "0000-0002-5075-5116" }, { "id": "Deppe-Nils", "name": { "family": "Deppe", "given": "Nils" }, "orcid": "0000-0003-4557-4115" }, { "id": "H\u00e9bert-Fran\u00e7ois", "name": { "family": "H\u00e9bert", "given": "Fran\u00e7ois" }, "orcid": "0000-0001-9009-6955" }, { "id": "Iozzo-Dante-A-B", "name": { "family": "Iozzo", "given": "Dante A.\u2009B." }, "orcid": "0000-0002-7244-1900" }, { "id": "Kidder-Lawrence-E", "name": { "family": "Kidder", "given": "Lawrence E." }, "orcid": "0000-0001-5392-7342" }, { "id": "Moxon-Jordan", "name": { "family": "Moxon", "given": "Jordan" }, "orcid": "0000-0001-9891-8677" }, { "id": "Pfeiffer-Harald-P", "name": { "family": "Pfeiffer", "given": "Harald P." }, "orcid": "0000-0001-9288-519X" }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." }, "orcid": "0000-0001-6656-9134" }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" }, { "id": "Throwe-William", "name": { "family": "Throwe", "given": "William" }, "orcid": "0000-0001-5059-4378" }, { "id": "Vu-Nils-L", "name": { "family": "Vu", "given": "Nils" }, "orcid": "0000-0002-5767-3949" } ] }, "title": "High precision ringdown modeling: Multimode fits and BMS frames", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2022 American Physical Society. \n\n(Received 11 November 2021; accepted 11 March 2022; published 11 May 2022) \n\nWe thank Max Isi for fruitful discussions, Matt Giesler for sharing his work, which helped us clarify the differences between our results and those of [18,19], and Arnab Dhani for detailed discussions on the methods used in his work [25]. We also thank Greg Cook, Arnab Dhani, Matt Giesler, Max Isi, and Xiang Li for reviewing an earlier version of this manuscript. Calculations were performed with the Wheeler cluster at the California Institute of Technology (Caltech), which is supported by the Sherman Fairchild Foundation and by Caltech. The work of L.\u2009M.\u2009Z. was partially supported by the MSSGC Graduate Research Fellowship, awarded through the NASA Cooperative Agreement No. 80NSSC20M0101. Part of this research was performed while L.\u2009M.\u2009Z. was visiting the Institute for Pure and Applied Mathematics (IPAM), which is supported by the National Science Foundation (Grant No. DMS-1925919) The work of K.\u2009M was partially supported by NSF Grants No. PHY-2011961, No. PHY-2011968, and No. OAC-1931266. The work of N.\u2009K. was partially supported by NSF Grant No. PHY-1806356, Grant No. UN2017-92945 from the Urania Stott Fund of the Pittsburgh Foundation, the Eberly research funds of Penn State at Penn State and the Mebus fellowship. The work of L.\u2009C.\u2009S. was partially supported by NSF CAREER Grant No. PHY\u20132047382. All plots were made using the python package matplotlib [80].\n\nPublished - PhysRevD.105.104015.pdf
Accepted Version - 2110.15922.pdf
", "abstract": "Quasinormal mode (QNM) modeling is an invaluable tool for characterizing remnant black holes, studying strong gravity, and testing general relativity. Only recently have QNM studies begun to focus on multimode fitting to numerical relativity strain waveforms. As gravitational wave observatories become even more sensitive they will be able to resolve higher-order modes. Consequently, multimode QNM fits will be critically important, and in turn require a more thorough treatment of the asymptotic frame at I\u207a. The first main result of this work is a method for systematically fitting a QNM model containing many modes to a numerical waveform produced using Cauchy-characteristic extraction (CCE), a waveform extraction technique which is known to resolve memory effects. We choose the modes to model based on their power contribution to the residual between numerical and model waveforms. We show that the all-mode strain mismatch improves by a factor of \u223c10\u2075 when using multimode fitting as opposed to only fitting the (2, \u00b12, n) modes. Our most significant result addresses a critical point that has been overlooked in the QNM literature: the importance of matching the Bondi-van der Burg-Metzner-Sachs (BMS) frame of the numerical waveform to that of the QNM model. We show that by mapping the numerical waveforms\u2014which exhibit the memory effect\u2014to a BMS frame known as the super rest frame, there is an improvement of \u223c10\u2075 in the all-mode strain mismatch compared to using a strain waveform whose BMS frame is not fixed. Furthermore, we find that by mapping CCE waveforms to the super rest frame, we can obtain all-mode mismatches that are, on average, a factor of \u223c4 better than using the publicly available extrapolated waveforms. We illustrate the effectiveness of these modeling enhancements by applying them to families of waveforms produced by numerical relativity and comparing our results to previous QNM studies.", "date": "2022-05-15", "date_type": "published", "publication": "Physical Review D", "volume": "105", "number": "10", "publisher": "American Physical Society", "pagerange": "Art. No. 104015", "id_number": "CaltechAUTHORS:20220601-257716000", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220601-257716000", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Sherman Fairchild Foundation" }, { "agency": "Caltech" }, { "agency": "Mississippi Space Grant Consortium", "grant_number": "80NSSC20M0101" }, { "agency": "NSF", "grant_number": "DMS-1925919" }, { "agency": "NSF", "grant_number": "PHY-2011961" }, { "agency": "NSF", "grant_number": "PHY-2011968" }, { "agency": "NSF", "grant_number": "OAC-1931266" }, { "agency": "NSF", "grant_number": "PHY-1806356" }, { "agency": "Pittsburgh Foundation", "grant_number": "UN2017-92945" }, { "agency": "NSF", "grant_number": "PHY-2047382" }, { "agency": "Pennsylvania State University" } ] }, "local_group": { "items": [ { "id": "TAPIR" } ] }, "doi": "10.1103/physrevd.105.104015", "primary_object": { "basename": "2110.15922.pdf", "url": "https://authors.library.caltech.edu/records/hhpz3-00q98/files/2110.15922.pdf" }, "related_objects": [ { "basename": "PhysRevD.105.104015.pdf", "url": "https://authors.library.caltech.edu/records/hhpz3-00q98/files/PhysRevD.105.104015.pdf" } ], "resource_type": "article", "pub_year": "2022", "author_list": "Maga\u00f1a Zertuche, Lorena; Mitman, Keefe; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/q9ne7-4q272", "eprint_id": 114680, "eprint_status": "archive", "datestamp": "2023-08-20 07:31:08", "lastmod": "2023-10-24 15:07:04", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Vu-Nils-L", "name": { "family": "Vu", "given": "Nils L." }, "orcid": "0000-0002-5767-3949" }, { "id": "Pfeiffer-Harald-P", "name": { "family": "Pfeiffer", "given": "Harald P." }, "orcid": "0000-0001-9288-519X" }, { "id": "Bonilla-Gabriel-S", "name": { "family": "Bonilla", "given": "Gabriel S." }, "orcid": "0000-0003-4502-528X" }, { "id": "Deppe-Nils", "name": { "family": "Deppe", "given": "Nils" }, "orcid": "0000-0003-4557-4115" }, { "id": "H\u00e9bert-Fran\u00e7ois", "name": { "family": "H\u00e9bert", "given": "Fran\u00e7ois" }, "orcid": "0000-0001-9009-6955" }, { "id": "Kidder-Lawrence-E", "name": { "family": "Kidder", "given": "Lawrence E." }, "orcid": "0000-0001-5392-7342" }, { "id": "Lovelace-Geoffrey", "name": { "family": "Lovelace", "given": "Geoffrey" }, "orcid": "0000-0002-7084-1070" }, { "id": "Moxon-Jordan", "name": { "family": "Moxon", "given": "Jordan" }, "orcid": "0000-0001-9891-8677" }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." }, "orcid": "0000-0001-6656-9134" }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" }, { "id": "Throwe-William", "name": { "family": "Throwe", "given": "William" }, "orcid": "0000-0001-5059-4378" }, { "id": "Wittek-Nikolas-A", "name": { "family": "Wittek", "given": "Nikolas A." }, "orcid": "0000-0001-8575-5450" }, { "id": "W\u0142odarczyk-Tom", "name": { "family": "W\u0142odarczyk", "given": "Tom" } } ] }, "title": "A scalable elliptic solver with task-based parallelism for the SpECTRE numerical relativity code", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2022 Published by the American Physical Society under the terms of the Creative Commons Attribution 4.0 International license. Further distribution of this work must maintain attribution to the author(s) and the published article's title, journal citation, and DOI. Open access publication funded by the Max Planck Society. \n\nReceived 15 November 2021; accepted 8 February 2022; published 18 April 2022. \n\nThe authors thank Tim Dietrich, Francois Foucart, and Hannes R\u00fcter for helpful discussions. N.\u2009V. also thanks the Cornell Center for Astrophysics and Planetary Science and TAPIR at Caltech for the hospitality and financial support during research stays. Computations were performed with the SpECTRE code [29] on the Minerva cluster at the Max Planck Institute for Gravitational Physics. Charm++ [38] was developed by the Parallel Programming Laboratory in the Department of Computer Science at the University of Illinois at Urbana-Champaign. The figures in this article were produced with dgpy [76], matplotlib [77,78], TikZ [79] and ParaView [80]. This work was supported in part by the Sherman Fairchild Foundation and by NSF Grants No. PHY-2011961, No. PHY-2011968, and No. OAC-1931266 at Caltech, and NSF Grants No. PHY-1912081 and No. OAC-1931280 at Cornell. G.\u2009L. is pleased to acknowledge support from the NSF through Grants No. PHY-1654359 and No. AST-1559694 and from Nicholas and Lee Begovich and the Dan Black Family Trust.\n\nPublished - PhysRevD.105.084027.pdf
Accepted Version - 2111.06767.pdf
Supplemental Material - Bbh.yaml
Supplemental Material - KerrSchild.yaml
Supplemental Material - Poisson.yaml
", "abstract": "Elliptic partial differential equations must be solved numerically for many problems in numerical relativity, such as initial data for every simulation of merging black holes and neutron stars. Existing elliptic solvers can take multiple days to solve these problems at high resolution and when matter is involved, because they are either hard to parallelize or require a large amount of computational resources. Here we present a new solver for linear and nonlinear elliptic problems that is designed to scale with resolution and to parallelize on computing clusters. To achieve this we employ a discontinuous Galerkin discretization, an iterative multigrid-Schwarz preconditioned Newton-Krylov algorithm, and a task-based parallelism paradigm. To accelerate convergence of the elliptic solver we have developed novel subdomain-preconditioning techniques. We find that our multigrid-Schwarz preconditioned elliptic solves achieve iteration counts that are independent of resolution, and our task-based parallel programs scale over 200 million degrees of freedom to at least a few thousand cores. Our new code solves a classic initial data problem for binary black holes faster than the spectral code SpEC when distributed to only eight cores, and in a fraction of the time on more cores. It is publicly accessible in the next-generation SpECTRE numerical relativity code. Our results pave the way for highly parallel elliptic solves in numerical relativity and beyond.", "date": "2022-04-15", "date_type": "published", "publication": "Physical Review D", "volume": "105", "number": "8", "publisher": "American Physical Society", "pagerange": "Art. No. 084027", "id_number": "CaltechAUTHORS:20220511-815710400", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220511-815710400", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Max Planck Society" }, { "agency": "Cornell University" }, { "agency": "Caltech" }, { "agency": "Sherman Fairchild Foundation" }, { "agency": "NSF", "grant_number": "PHY-2011961" }, { "agency": "NSF", "grant_number": "PHY-2011968" }, { "agency": "NSF", "grant_number": "OAC-1931266" }, { "agency": "NSF", "grant_number": "PHY-1912081" }, { "agency": "NSF", "grant_number": "OAC-1931280" }, { "agency": "NSF", "grant_number": "PHY-1654359" }, { "agency": "NSF", "grant_number": "AST-1559694" }, { "agency": "Nicholas and Lee Begovich" }, { "agency": "Dan Black Family Trust" } ] }, "local_group": { "items": [ { "id": "TAPIR" }, { "id": "Walter-Burke-Institute-for-Theoretical-Physics" } ] }, "doi": "10.1103/physrevd.105.084027", "primary_object": { "basename": "KerrSchild.yaml", "url": "https://authors.library.caltech.edu/records/q9ne7-4q272/files/KerrSchild.yaml" }, "related_objects": [ { "basename": "PhysRevD.105.084027.pdf", "url": "https://authors.library.caltech.edu/records/q9ne7-4q272/files/PhysRevD.105.084027.pdf" }, { "basename": "Poisson.yaml", "url": "https://authors.library.caltech.edu/records/q9ne7-4q272/files/Poisson.yaml" }, { "basename": "2111.06767.pdf", "url": "https://authors.library.caltech.edu/records/q9ne7-4q272/files/2111.06767.pdf" }, { "basename": "Bbh.yaml", "url": "https://authors.library.caltech.edu/records/q9ne7-4q272/files/Bbh.yaml" } ], "resource_type": "article", "pub_year": "2022", "author_list": "Vu, Nils L.; Pfeiffer, Harald P.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/r2eap-s9f26", "eprint_id": 111454, "eprint_status": "archive", "datestamp": "2023-08-20 05:37:01", "lastmod": "2023-10-23 15:32:54", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Chen-Yitian", "name": { "family": "Chen", "given": "Yitian" }, "orcid": "0000-0002-8664-9702" }, { "id": "Deppe-Nils", "name": { "family": "Deppe", "given": "Nils" }, "orcid": "0000-0003-4557-4115" }, { "id": "Kidder-Lawrence-E", "name": { "family": "Kidder", "given": "Lawrence E." }, "orcid": "0000-0001-5392-7342" }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Efficient simulations of high-spin black holes with a new gauge", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2021 American Physical Society. \n\n(Received 6 August 2021; accepted 21 September 2021; published 12 October 2021) \n\nWe thank Michael Boyle, Dante Iozzo, and Vijay Varma for useful discussions. Computations were performed with the High Performance Computing Center and the Wheeler cluster at Caltech. Computations were also conducted on the Frontera computing project at the Texas Advanced Computing Center. This work was supported in part by the Sherman Fairchild Foundation and by NSF Grants No. PHY-2011961, No. PHY-2011968, and No. OAC-1931266 at Caltech, and NSF Grants No. PHY-1912081 and No. OAC-1931280 at Cornell.\n\nPublished - PhysRevD.104.084046.pdf
Submitted - 2108.02331.pdf
", "abstract": "We present a new choice of initial data for binary black hole simulations that significantly improves the efficiency of high-spin simulations. We use spherical Kerr-Schild coordinates, where the horizon of a rotating black hole is spherical, for each black hole. The superposed spherical Kerr-Schild initial data reduce the runtime by a factor of 2 compared to standard superposed Kerr-Schild for an intermediate resolution spin-0.99 binary-black-hole simulation. We also explore different variations of the gauge conditions imposed during the evolution, one of which produces an additional speed-up of 1.3.", "date": "2021-10-15", "date_type": "published", "publication": "Physical Review D", "volume": "104", "number": "8", "publisher": "American Physical Society", "pagerange": "Art. No. 084046", "id_number": "CaltechAUTHORS:20211014-212144369", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20211014-212144369", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Sherman Fairchild Foundation" }, { "agency": "NSF", "grant_number": "PHY-2011961" }, { "agency": "NSF", "grant_number": "PHY-2011968" }, { "agency": "NSF", "grant_number": "OAC-1931266" }, { "agency": "NSF", "grant_number": "PHY-1912081" }, { "agency": "NSF", "grant_number": "OAC-1931280" } ] }, "local_group": { "items": [ { "id": "TAPIR" } ] }, "doi": "10.1103/PhysRevD.104.084046", "primary_object": { "basename": "2108.02331.pdf", "url": "https://authors.library.caltech.edu/records/r2eap-s9f26/files/2108.02331.pdf" }, "related_objects": [ { "basename": "PhysRevD.104.084046.pdf", "url": "https://authors.library.caltech.edu/records/r2eap-s9f26/files/PhysRevD.104.084046.pdf" } ], "resource_type": "article", "pub_year": "2021", "author_list": "Chen, Yitian; Deppe, Nils; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/rch9y-wt729", "eprint_id": 110367, "eprint_status": "archive", "datestamp": "2023-08-20 04:15:57", "lastmod": "2023-10-23 19:37:06", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Mitman-Keefe", "name": { "family": "Mitman", "given": "Keefe" }, "orcid": "0000-0003-0276-3856" }, { "id": "Khera-Neev", "name": { "family": "Khera", "given": "Neev" }, "orcid": "0000-0003-3515-2859" }, { "id": "Iozzo-Dante-A-B", "name": { "family": "Iozzo", "given": "Dante A.\u2009B." }, "orcid": "0000-0002-7244-1900" }, { "id": "Stein-Leo-C", "name": { "family": "Stein", "given": "Leo C." }, "orcid": "0000-0001-7559-9597" }, { "id": "Boyle-Michael", "name": { "family": "Boyle", "given": "Michael" }, "orcid": "0000-0002-5075-5116" }, { "id": "Deppe-Nils", "name": { "family": "Deppe", "given": "Nils" }, "orcid": "0000-0003-4557-4115" }, { "id": "Kidder-Lawrence-E", "name": { "family": "Kidder", "given": "Lawrence E." }, "orcid": "0000-0001-5392-7342" }, { "id": "Moxon-Jordan", "name": { "family": "Moxon", "given": "Jordan" }, "orcid": "0000-0001-9891-8677" }, { "id": "Pfeiffer-Harald-P", "name": { "family": "Pfeiffer", "given": "Harald P." }, "orcid": "0000-0001-9288-519X" }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." }, "orcid": "0000-0001-6656-9134" }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" }, { "id": "Throwe-William", "name": { "family": "Throwe", "given": "William" }, "orcid": "0000-0001-5059-4378" } ] }, "title": "Fixing the BMS frame of numerical relativity waveforms", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2021 American Physical Society. \n\nReceived 11 May 2021; accepted 17 June 2021; published 20 July 2021. \n\nComputations were performed with the High Performance Computing Center and the Wheeler cluster at Caltech. This work was supported in part by the Sherman Fairchild Foundation and by NSF Grants No. PHY-2011961, No. PHY-2011968, and No. OAC-1931266 at Caltech, NSF Grants No. PHY-1912081 and No. OAC-1931280 at Cornell, and NSF Grant No. PHY-1806356, Grant No. UN2017-92945 from the Urania Stott Fund of the Pittsburgh Foundation, and the Eberly research funds of Penn State at Penn State.\n\nPublished - PhysRevD.104.024051.pdf
Accepted Version - 2105.02300.pdf
", "abstract": "Understanding the Bondi-Metzner-Sachs (BMS) frame of the gravitational waves produced by numerical relativity is crucial for ensuring that analyses on such waveforms are performed properly. It is also important that models are built from waveforms in the same BMS frame. Up until now, however, the BMS frame of numerical waveforms has not been thoroughly examined, largely because the necessary tools have not existed. In this paper, we show how to analyze and map to a suitable BMS frame for numerical waveforms calculated with the Spectral Einstein Code (SpEC). However, the methods and tools that we present are general and can be applied to any numerical waveforms. We present an extensive study of 13 binary black hole systems that broadly span parameter space. From these simulations, we extract the strain and also the Weyl scalars using both SpECTRE's Cauchy-characteristic extraction module and also the standard extrapolation procedure with a displacement memory correction applied during postprocessing. First, we show that the current center-of-mass correction used to map these waveforms to the center-of-mass frame is not as effective as previously thought. Consequently, we also develop an improved correction that utilizes asymptotic Poincar\u00e9 charges instead of a Newtonian center-of-mass trajectory. Next, we map our waveforms to the post-Newtonian (PN) BMS frame using a PN strain waveform. This helps us find the unique BMS transformation that minimizes the L\u00b2 norm of the difference between the numerical and PN strain waveforms during the early inspiral phase. We find that once the waveforms are mapped to the PN BMS frame, they can be hybridized with a PN strain waveform much more effectively than if one used any of the previous alignment schemes, which only utilize the Poincar\u00e9 transformations.", "date": "2021-07-15", "date_type": "published", "publication": "Physical Review D", "volume": "104", "number": "2", "publisher": "American Physical Society", "pagerange": "Art. No. 024051", "id_number": "CaltechAUTHORS:20210821-163947559", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210821-163947559", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Sherman Fairchild Foundation" }, { "agency": "NSF", "grant_number": "PHY-2011961" }, { "agency": "NSF", "grant_number": "PHY-2011968" }, { "agency": "NSF", "grant_number": "OAC-1931266" }, { "agency": "NSF", "grant_number": "PHY-1912081" }, { "agency": "NSF", "grant_number": "OAC-1931280" }, { "agency": "NSF", "grant_number": "PHY-1806356" }, { "agency": "Pittsburgh Foundation", "grant_number": "UN2017-92945" }, { "agency": "Pennsylvania State University" } ] }, "local_group": { "items": [ { "id": "TAPIR" } ] }, "doi": "10.1103/physrevd.104.024051", "primary_object": { "basename": "2105.02300.pdf", "url": "https://authors.library.caltech.edu/records/rch9y-wt729/files/2105.02300.pdf" }, "related_objects": [ { "basename": "PhysRevD.104.024051.pdf", "url": "https://authors.library.caltech.edu/records/rch9y-wt729/files/PhysRevD.104.024051.pdf" } ], "resource_type": "article", "pub_year": "2021", "author_list": "Mitman, Keefe; Khera, Neev; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/500mw-h3g71", "eprint_id": 109763, "eprint_status": "archive", "datestamp": "2023-08-20 04:07:16", "lastmod": "2023-10-23 18:09:27", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Isi-Maximiliano", "name": { "family": "Isi", "given": "Maximiliano" }, "orcid": "0000-0001-8830-8672" }, { "id": "Farr-Will-M", "name": { "family": "Farr", "given": "Will M." }, "orcid": "0000-0003-1540-8562" }, { "id": "Giesler-Matthew-D", "name": { "family": "Giesler", "given": "Matthew" }, "orcid": "0000-0003-2300-893X" }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." }, "orcid": "0000-0001-6656-9134" }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Testing the Black-Hole Area Law with GW150914", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2021 American Physical Society. \n\n(Received 8 December 2020; accepted 26 May 2021; published 1 July 2021) \n\nWe thank Kip S. Thorne for encouraging this study and providing feedback during its development; we also thank Geraint Pratten, Nathan Johnson-McDaniel, and Katerina Chatziioannou for comments on the draft. M.\u2009I. is supported by NASA through the NASA Hubble Fellowship Grant No. HST-HF2-51410.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under Contract NAS5-26555. The Flatiron Institute is supported by the Simons Foundation. M.\u2009G. and S.\u2009T. are supported in part by the Sherman Fairchild Foundation and by NSF Grant No. PHY-1912081 at Cornell. M.\u2009S. is supported in part by the Sherman Fairchild Foundation and NSF Grants No. PHY-2011961 and No. PHY-2011968 at Caltech. This research has made use of data, software, and/or web tools obtained from the Gravitational Wave Open Science Center [29], a service of LIGO Laboratory, the LIGO Scientific Collaboration, and the Virgo Collaboration. LIGO Laboratory and Advanced LIGO are funded by the United States National Science Foundation (NSF) as well as the Science and Technology Facilities Council (STFC) of the United Kingdom, the Max-Planck-Society (MPS), and the State of Niedersachsen/Germany for support of the construction of Advanced LIGO and construction and operation of the GEO600 detector. Additional support for Advanced LIGO was provided by the Australian Research Council. Virgo is funded, through the European Gravitational Observatory (EGO), by the French Centre National de Recherche Scientifique (CNRS), the Italian Istituto Nazionale della Fisica Nucleare (INFN), and the Dutch Nikhef, with contributions by institutions from Belgium, Germany, Greece, Hungary, Ireland, Japan, Monaco, Poland, Portugal, and Spain. The authors are grateful for computational resources provided by the LIGO Laboratory and Cardiff University, and supported by NSF Grants No. PHY-0757058 and No. PHY-0823459, and STFC Grant No. ST/I006285/1. This Letter carries LIGO document number LIGO-P2000507.\n\nPublished - PhysRevLett.127.011103.pdf
Accepted Version - 2012.04486.pdf
", "abstract": "We present observational confirmation of Hawking's black-hole area theorem based on data from GW150914, finding agreement with the prediction with 97% (95%) probability when we model the ringdown including (excluding) overtones of the quadrupolar mode. We obtain this result from a new time-domain analysis of the pre- and postmerger data. We also confirm that the inspiral and ringdown portions of the signal are consistent with the same remnant mass and spin, in agreement with general relativity.", "date": "2021-07-01", "date_type": "published", "publication": "Physical Review Letters", "volume": "127", "number": "1", "publisher": "American Physical Society", "pagerange": "Art. No. 011103", "id_number": "CaltechAUTHORS:20210709-212641325", "issn": "0031-9007", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210709-212641325", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF2-51410.001-A" }, { "agency": "NASA", "grant_number": "NAS5-26555" }, { "agency": "Simons Foundation" }, { "agency": "Sherman Fairchild Foundation" }, { "agency": "NSF", "grant_number": "PHY-1912081" }, { "agency": "NSF", "grant_number": "PHY-2011961" }, { "agency": "NSF", "grant_number": "PHY-2011968" }, { "agency": "Max-Planck-Society" }, { "agency": "Australian Research Council" }, { "agency": "European Gravitational Observatory (EGO)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Istituto Nazionale di Fisica Nucleare (INFN)" }, { "agency": "Dutch National Institute for Subatomic Physics" }, { "agency": "NSF", "grant_number": "PHY-0757058" }, { "agency": "NSF", "grant_number": "PHY-0823459" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/I006285/1" } ] }, "other_numbering_system": { "items": [ { "id": "P2000507", "name": "LIGO Document" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" }, { "id": "TAPIR" }, { "id": "LIGO" } ] }, "doi": "10.1103/physrevlett.127.011103", "primary_object": { "basename": "2012.04486.pdf", "url": "https://authors.library.caltech.edu/records/500mw-h3g71/files/2012.04486.pdf" }, "related_objects": [ { "basename": "PhysRevLett.127.011103.pdf", "url": "https://authors.library.caltech.edu/records/500mw-h3g71/files/PhysRevLett.127.011103.pdf" } ], "resource_type": "article", "pub_year": "2021", "author_list": "Isi, Maximiliano; Farr, Will M.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/6073c-fe650", "eprint_id": 109551, "eprint_status": "archive", "datestamp": "2023-08-20 03:42:27", "lastmod": "2023-10-23 18:02:36", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Iozzo-Dante-A-B", "name": { "family": "Iozzo", "given": "Dante A.\u2009B." }, "orcid": "0000-0002-7244-1900" }, { "id": "Khera-Neev", "name": { "family": "Khera", "given": "Neev" }, "orcid": "0000-0003-3515-2859" }, { "id": "Stein-Leo-C", "name": { "family": "Stein", "given": "Leo C." }, "orcid": "0000-0001-7559-9597" }, { "id": "Mitman-Keefe", "name": { "family": "Mitman", "given": "Keefe" }, "orcid": "0000-0003-0276-3856" }, { "id": "Boyle-Michael", "name": { "family": "Boyle", "given": "Michael" }, "orcid": "0000-0002-5075-5116" }, { "id": "Deppe-Nils", "name": { "family": "Deppe", "given": "Nils" }, "orcid": "0000-0003-4557-4115" }, { "id": "H\u00e9bert-Fran\u00e7ois", "name": { "family": "H\u00e9bert", "given": "Fran\u00e7ois" }, "orcid": "0000-0001-9009-6955" }, { "id": "Kidder-Lawrence-E", "name": { "family": "Kidder", "given": "Lawrence E." }, "orcid": "0000-0001-5392-7342" }, { "id": "Moxon-Jordan", "name": { "family": "Moxon", "given": "Jordan" }, "orcid": "0000-0001-9891-8677" }, { "id": "Pfeiffer-Harald-P", "name": { "family": "Pfeiffer", "given": "Harald P." }, "orcid": "0000-0001-9288-519X" }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." }, "orcid": "0000-0001-6656-9134" }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" }, { "id": "Throwe-William", "name": { "family": "Throwe", "given": "William" }, "orcid": "0000-0001-5059-4378" } ] }, "title": "Comparing remnant properties from horizon data and asymptotic data in numerical relativity", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2021 American Physical Society. \n\nReceived 14 April 2021; accepted 3 May 2021; published 10 June 2021. \n\nThe authors would like to thank Kartik Prabhu and Vijay Varma for useful discussions. Computations were performed with the High Performance Computing Center and the Wheeler cluster at Caltech. This work was supported in part by the Sherman Fairchild Foundation and by NSF Grants No. PHY-2011961, No. PHY-2011968, and No. OAC-1931266 at Caltech, NSF Grants No. PHY-1912081 and No. OAC-1931280 at Cornell, and NSF Grants No. PHY-1806356, No. UN2017-92945 from the Urania Stott Fund of the Pittsburgh Foundation, and the Eberly research funds of Penn State at Penn State.\n\nPublished - PhysRevD.103.124029.pdf
Accepted Version - 2104.07052.pdf
", "abstract": "We present a new study of remnant black hole properties from 13 binary black hole systems, numerically evolved using the Spectral Einstein Code. The mass, spin, and recoil velocity of each remnant were determined quasilocally from apparent horizon data and asymptotically from Bondi data (h,\u03c8\u2084,\u03c8\u2083,\u03c8\u2082,\u03c8\u2081) computed at future null infinity using SpECTRE's Cauchy characteristic evolution. We compare these independent measurements of the remnant properties in the bulk and on the boundary of the spacetime, giving insight into how well asymptotic data are able to reproduce local properties of the remnant black hole in numerical relativity. We also discuss the theoretical framework for connecting horizon quantities to asymptotic quantities and how it relates to our results. This study recommends a simple improvement to the recoil velocities reported in the Simulating eXtreme Spacetimes waveform catalog, provides an improvement to future surrogate remnant models, and offers new analysis techniques for evaluating the physical accuracy of numerical simulations.", "date": "2021-06-15", "date_type": "published", "publication": "Physical Review D", "volume": "103", "number": "12", "publisher": "American Physical Society", "pagerange": "Art. No. 124029", "id_number": "CaltechAUTHORS:20210623-155717011", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210623-155717011", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Sherman Fairchild Foundation" }, { "agency": "NSF", "grant_number": "PHY-2011961" }, { "agency": "NSF", "grant_number": "PHY-2011968" }, { "agency": "NSF", "grant_number": "OAC-1931266" }, { "agency": "NSF", "grant_number": "PHY-1912081" }, { "agency": "NSF", "grant_number": "OAC-1931280" }, { "agency": "NSF", "grant_number": "PHY-1806356" }, { "agency": "Pittsburgh Foundation", "grant_number": "UN2017-92945" }, { "agency": "Pennsylvania State University" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" }, { "id": "TAPIR" } ] }, "doi": "10.1103/physrevd.103.124029", "primary_object": { "basename": "2104.07052.pdf", "url": "https://authors.library.caltech.edu/records/6073c-fe650/files/2104.07052.pdf" }, "related_objects": [ { "basename": "PhysRevD.103.124029.pdf", "url": "https://authors.library.caltech.edu/records/6073c-fe650/files/PhysRevD.103.124029.pdf" } ], "resource_type": "article", "pub_year": "2021", "author_list": "Iozzo, Dante A.\u2009B.; Khera, Neev; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/nf2zc-rqn39", "eprint_id": 107628, "eprint_status": "archive", "datestamp": "2023-08-20 01:28:18", "lastmod": "2023-10-23 16:04:10", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Iozzo-Dante-A-B", "name": { "family": "Iozzo", "given": "Dante A.\u2009B." }, "orcid": "0000-0002-7244-1900" }, { "id": "Boyle-Michael", "name": { "family": "Boyle", "given": "Michael" }, "orcid": "0000-0002-5075-5116" }, { "id": "Deppe-Nils", "name": { "family": "Deppe", "given": "Nils" }, "orcid": "0000-0003-4557-4115" }, { "id": "Moxon-Jordan", "name": { "family": "Moxon", "given": "Jordan" }, "orcid": "0000-0001-9891-8677" }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." }, "orcid": "0000-0001-6656-9134" }, { "id": "Kidder-Lawrence-E", "name": { "family": "Kidder", "given": "Lawrence E." }, "orcid": "0000-0001-5392-7342" }, { "id": "Pfeiffer-Harald-P", "name": { "family": "Pfeiffer", "given": "Harald P." }, "orcid": "0000-0001-9288-519X" }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Extending gravitational wave extraction using Weyl characteristic fields", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2021 American Physical Society. \n\n(Received 29 October 2020; accepted 22 December 2020; published 20 January 2021) \n\nWe are grateful to Will Throwe, Eamonn O'Shea, Crist\u00f3bal Armaza, and Gabriel Bonilla for insightful discussions. Computations were performed with the High Performance Computing Center and the Wheeler cluster at Caltech. This work was supported in part by the Sherman Fairchild Foundation and by NSF Grants No. PHY-2011961, No. PHY-2011968, and No. OAC-1931266 at Caltech and NSF Grants No. PHY-1912081 and No. OAC-1931280 at Cornell.\n\nPublished - PhysRevD.103.024039.pdf
Accepted Version - 2010.15200.pdf
", "abstract": "We present a detailed methodology for extracting the full set of Newman-Penrose Weyl scalars from numerically generated spacetimes without requiring a tetrad that is completely orthonormal or perfectly aligned to the principal null directions. We also describe how to implement an extrapolation technique for computing the Weyl scalars' contribution at asymptotic null infinity in postprocessing. These methods have been used to produce \u03a8\u2084 and \u210e waveforms for the Simulating eXtreme Spacetimes (SXS) waveform catalog and now have been expanded to produce the entire set of Weyl scalars. These new waveform quantities are critical for the future of gravitational wave astronomy in order to understand the finite-amplitude gauge differences that can occur in numerical waveforms. We also present a new analysis of the accuracy of waveforms produced by the Spectral Einstein Code. While ultimately we expect Cauchy characteristic extraction to yield more accurate waveforms, the extraction techniques described here are far easier to implement and have already proven to be a viable way to produce production-level waveforms that can meet the demands of current gravitational-wave detectors.", "date": "2021-01-20", "date_type": "published", "publication": "Physical Review D", "volume": "103", "number": "2", "publisher": "American Physical Society", "pagerange": "Art. No. 024039", "id_number": "CaltechAUTHORS:20210121-101410882", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210121-101410882", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Sherman Fairchild Foundation" }, { "agency": "NSF", "grant_number": "PHY-2011961" }, { "agency": "NSF", "grant_number": "PHY-2011968" }, { "agency": "NSF", "grant_number": "OAC-1931266" }, { "agency": "NSF", "grant_number": "PHY-1912081" }, { "agency": "NSF", "grant_number": "OAC-1931280" } ] }, "doi": "10.1103/physrevd.103.024039", "primary_object": { "basename": "2010.15200.pdf", "url": "https://authors.library.caltech.edu/records/nf2zc-rqn39/files/2010.15200.pdf" }, "related_objects": [ { "basename": "PhysRevD.103.024039.pdf", "url": "https://authors.library.caltech.edu/records/nf2zc-rqn39/files/PhysRevD.103.024039.pdf" } ], "resource_type": "article", "pub_year": "2021", "author_list": "Iozzo, Dante A.\u2009B.; Boyle, Michael; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/3yyxr-bjy13", "eprint_id": 107408, "eprint_status": "archive", "datestamp": "2023-08-20 01:25:22", "lastmod": "2023-10-23 15:51:38", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Mitman-Keefe", "name": { "family": "Mitman", "given": "Keefe" }, "orcid": "0000-0003-0276-3856" }, { "id": "Iozzo-Dante-A-B", "name": { "family": "Iozzo", "given": "Dante A. B." } }, { "id": "Khera-Neev", "name": { "family": "Khera", "given": "Neev" } }, { "id": "Boyle-Michael", "name": { "family": "Boyle", "given": "Michael" }, "orcid": "0000-0002-5075-5116" }, { "id": "De-Lorenzo-Tommaso", "name": { "family": "De Lorenzo", "given": "Tommaso" } }, { "id": "Deppe-Nils", "name": { "family": "Deppe", "given": "Nils" }, "orcid": "0000-0003-4557-4115" }, { "id": "Kidder-Lawrence-E", "name": { "family": "Kidder", "given": "Lawrence E." }, "orcid": "0000-0001-5392-7342" }, { "id": "Moxon-Jordan", "name": { "family": "Moxon", "given": "Jordan" }, "orcid": "0000-0001-9891-8677" }, { "id": "Pfeiffer-Harald-P", "name": { "family": "Pfeiffer", "given": "Harald P." }, "orcid": "0000-0001-9288-519X" }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." }, "orcid": "0000-0001-6656-9134" }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" }, { "id": "Throwe-William", "name": { "family": "Throwe", "given": "William" }, "orcid": "0000-0001-5059-4378" } ] }, "title": "Adding gravitational memory to waveform catalogs using BMS balance laws", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2021 American Physical Society. \n\nReceived 4 November 2020; accepted 21 December 2020; published 15 January 2021. \n\nWe would like to thank Dennis Pollney for sharing data that was used in the early stages of this project. Computations were performed with the High Performance Computing Center and on the Wheeler cluster at Caltech, which is supported by the Sherman Fairchild Foundation and by Caltech. This work was supported in part by the Sherman Fairchild Foundation and by NSF Grants No. PHY-2011961, No. PHY-2011968, and No. OAC-1931266 at Caltech, NSF Grants No. PHY-1912081 and No. OAC-1931280 at Cornell, and NSF Grant No. PHY-1806356, Grant No. UN2017-92945 from the Urania Stott Fund of the Pittsburgh Foundation, and the Eberly research funds of Penn State at Penn State.\n\nPublished - PhysRevD.103.024031.pdf
Submitted - 2011.01309.pdf
Supplemental Material - Memory.ipynb
", "abstract": "Accurate models of gravitational waves from merging binary black holes are crucial for detectors to measure events and extract new science. One important feature that is currently missing from the Simulating eXtreme Spacetimes (SXS) Collaboration's catalog of waveforms for merging black holes, and other waveform catalogs, is the gravitational memory effect: a persistent, physical change to spacetime that is induced by the passage of transient radiation. We find, however, that by exploiting the Bondi-van der Burg-Metzner-Sachs (BMS) balance laws, which come from the extended BMS transformations, we can correct the strain waveforms in the SXS catalog to include the missing displacement memory. Our results show that these corrected waveforms satisfy the BMS balance laws to a much higher degree of accuracy. Furthermore, we find that these corrected strain waveforms coincide especially well with the waveforms obtained from Cauchy-characteristic extraction (CCE) that already exhibit memory effects. These corrected strain waveforms also evade the transient junk effects that are currently present in CCE waveforms. Last, we make our code for computing these contributions to the BMS balance laws and memory publicly available as a part of the python package sxs, thus enabling anyone to evaluate the expected memory effects and violation of the BMS balance laws.", "date": "2021-01-15", "date_type": "published", "publication": "Physical Review D", "volume": "103", "number": "2", "publisher": "American Physical Society", "pagerange": "Art. No. 024031", "id_number": "CaltechAUTHORS:20210111-160852376", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210111-160852376", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Sherman Fairchild Foundation" }, { "agency": "Caltech" }, { "agency": "NSF", "grant_number": "PHY-2011961" }, { "agency": "NSF", "grant_number": "PHY-2011968" }, { "agency": "NSF", "grant_number": "OAC-1931266" }, { "agency": "NSF", "grant_number": "PHY-1912081" }, { "agency": "NSF", "grant_number": "OAC-1931280" }, { "agency": "NSF", "grant_number": "PHY-1806356" }, { "agency": "Pittsburgh Foundation", "grant_number": "UN2017-92945" }, { "agency": "Pennsylvania State University" } ] }, "local_group": { "items": [ { "id": "TAPIR" }, { "id": "Walter-Burke-Institute-for-Theoretical-Physics" } ] }, "doi": "10.1103/PhysRevD.103.024031", "primary_object": { "basename": "Memory.ipynb", "url": "https://authors.library.caltech.edu/records/3yyxr-bjy13/files/Memory.ipynb" }, "related_objects": [ { "basename": "PhysRevD.103.024031.pdf", "url": "https://authors.library.caltech.edu/records/3yyxr-bjy13/files/PhysRevD.103.024031.pdf" }, { "basename": "2011.01309.pdf", "url": "https://authors.library.caltech.edu/records/3yyxr-bjy13/files/2011.01309.pdf" } ], "resource_type": "article", "pub_year": "2021", "author_list": "Mitman, Keefe; Iozzo, Dante A. B.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/tt53n-7pf81", "eprint_id": 98091, "eprint_status": "archive", "datestamp": "2023-08-20 00:44:50", "lastmod": "2023-10-18 17:02:09", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Throwe-William", "name": { "family": "Throwe", "given": "William" }, "orcid": "0000-0001-5059-4378" }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul" }, "orcid": "0000-0001-9765-4526" } ] }, "title": "A High-Order, Conservative Integrator with Local Time-Stepping", "ispublished": "pub", "full_text_status": "public", "keywords": "local time-stepping, multirate time integration, Adams methods, adaptive time stepping, conservation laws", "note": "\u00a9 2020 Society for Industrial and Applied Mathematics. \n\nSubmitted to the journal's Methods and Algorithms for Scientific Computing section October 11, 2019; accepted for publication (in revised form) September 21, 2020; published electronically December 1, 2020. \n\nThis work was partially supported by the Sherman Fairchild Foundation and by NSF through grants PHY-1606654 and ACI-1713678.\n\nPublished - 19m1292692.pdf
Submitted - 1811.02499.pdf
", "abstract": "We present a family of multistep integrators based on the Adams--Bashforth methods. These schemes can be constructed for arbitrary convergence order with arbitrary step size variation. The step size can differ between different subdomains of the system. It can also change with time within a given subdomain. The methods are linearly conservative, preserving a wide class of analytically constant quantities to numerical roundoff, even when numerical truncation error is significantly higher. These methods are intended for use in solving conservative PDEs in discontinuous Galerkin formulations or in finite-difference methods with compact stencils. A numerical test demonstrates these properties and shows that significant speed improvements over the standard Adams--Bashforth schemes can be obtained.", "date": "2020-12-01", "date_type": "published", "publication": "SIAM Journal on Scientific Computing", "volume": "42", "number": "6", "publisher": "Society for Industrial and Applied Mathematics", "pagerange": "A3730-A3760", "id_number": "CaltechAUTHORS:20190821-155551404", "issn": "1064-8275", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190821-155551404", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Sherman Fairchild Foundation" }, { "agency": "NSF", "grant_number": "PHY-1606654" }, { "agency": "NSF", "grant_number": "ACI-1713678" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.1137/19M1292692", "primary_object": { "basename": "1811.02499.pdf", "url": "https://authors.library.caltech.edu/records/tt53n-7pf81/files/1811.02499.pdf" }, "related_objects": [ { "basename": "19m1292692.pdf", "url": "https://authors.library.caltech.edu/records/tt53n-7pf81/files/19m1292692.pdf" } ], "resource_type": "article", "pub_year": "2020", "author_list": "Throwe, William and Teukolsky, Saul" }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/pars6-dky03", "eprint_id": 106431, "eprint_status": "archive", "datestamp": "2023-08-20 00:22:47", "lastmod": "2023-10-20 23:28:55", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Mitman-K", "name": { "family": "Mitman", "given": "Keefe" }, "orcid": "0000-0003-0276-3856" }, { "id": "Moxon-J", "name": { "family": "Moxon", "given": "Jordan" }, "orcid": "0000-0001-9891-8677" }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" }, { "id": "Boyle-M", "name": { "family": "Boyle", "given": "Michael" } }, { "id": "Deppe-N", "name": { "family": "Deppe", "given": "Nils" } }, { "id": "Kidder-L-E", "name": { "family": "Kidder", "given": "Lawrence E." }, "orcid": "0000-0001-5392-7342" }, { "id": "Throwe-W", "name": { "family": "Throwe", "given": "William" } } ] }, "title": "Computation of displacement and spin gravitational memory in numerical relativity", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2020 American Physical Society. \n\nReceived 23 July 2020; accepted 2 October 2020; published 2 November 2020. \n\nWe thank Matt Giesler for many useful conversations. Computations were performed on the Wheeler cluster at the California Institute of Technology (Caltech), which is supported by the Sherman Fairchild Foundation and by Caltech. This work was supported in part by the Sherman Fairchild Foundation and by NSF Grants No. PHY-1708212, No. PHY-1708213, and No. OAC-1931266 at Caltech and NSF Grants No. PHY-1912081 and No. OAC-1931280 at Cornell.\n\nPublished - PhysRevD.102.104007.pdf
", "abstract": "We present the first numerical relativity waveforms for binary black hole mergers produced using spectral methods that show both the displacement and the spin memory effects. Explicitly, we use the SXS (Simulating eXtreme Spacetimes) Collaboration's SpEC code to run a Cauchy evolution of a binary black hole merger and then extract the gravitational wave strain using SpECTRE's version of a Cauchy-characteristic extraction. We find that we can accurately resolve the strain's traditional m=0 memory modes and some of the m\u22600 oscillatory memory modes that have previously only been theorized. We also perform a separate calculation of the memory using equations for the Bondi-Metzner-Sachs charges as well as the energy and angular momentum fluxes at asymptotic infinity. Our new calculation uses only the gravitational wave strain and two of the Weyl scalars at infinity. Also, this computation shows that the memory modes can be understood as a combination of a memory signal throughout the binary's inspiral and merger phases, and a quasinormal mode signal near the ringdown phase. Additionally, we find that the magnetic memory, up to numerical error, is indeed zero as previously conjectured. Last, we find that signal-to-noise ratios of memory for LIGO, the Einstein Telescope, and the Laser Interferometer Space Antenna with these new waveforms and new memory calculation are larger than previous expectations based on post-Newtonian or minimal waveform models.", "date": "2020-11-15", "date_type": "published", "publication": "Physical Review D", "volume": "102", "number": "10", "publisher": "American Physical Society", "pagerange": "Art. No. 104007", "id_number": "CaltechAUTHORS:20201104-132612504", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20201104-132612504", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Sherman Fairchild Foundation" }, { "agency": "Caltech" }, { "agency": "NSF", "grant_number": "PHY-1708212" }, { "agency": "NSF", "grant_number": "PHY-1708213" }, { "agency": "NSF", "grant_number": "OAC-1931266" }, { "agency": "NSF", "grant_number": "PHY-1912081" }, { "agency": "NSF", "grant_number": "OAC-1931280" } ] }, "local_group": { "items": [ { "id": "TAPIR" }, { "id": "Walter-Burke-Institute-for-Theoretical-Physics" } ] }, "doi": "10.1103/physrevd.102.104007", "primary_object": { "basename": "PhysRevD.102.104007.pdf", "url": "https://authors.library.caltech.edu/records/pars6-dky03/files/PhysRevD.102.104007.pdf" }, "resource_type": "article", "pub_year": "2020", "author_list": "Mitman, Keefe; Moxon, Jordan; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/xzcne-vwg56", "eprint_id": 105195, "eprint_status": "archive", "datestamp": "2023-08-19 22:58:11", "lastmod": "2023-10-20 21:27:26", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Moxon-J", "name": { "family": "Moxon", "given": "Jordan" }, "orcid": "0000-0001-9891-8677" }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Improved Cauchy-characteristic evolution system for high-precision numerical relativity waveforms", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2020 American Physical Society. \n\nReceived 6 July 2020; accepted 24 July 2020; published 28 August 2020. \n\nWe thank Kevin Barkett, Michael Boyle, Dante Iozzo, Bela Szilagyi, and Jeff Winicour for valuable discussions and suggestions regarding this project. We thank Harald Pfeiffer for suggestions improving the presentation in this paper. This work was supported in part by the Sherman Fairchild Foundation and by NSF Grants No. PHY-1708212, No. PHY-1708213, and No. OAC-1931266 at Caltech and NSF Grants No. PHY-1912081 and No. OAC-1931280 at Cornell.\n\nPublished - PhysRevD.102.044052.pdf
Submitted - 2007.01339.pdf
", "abstract": "We present several improvements to the Cauchy-characteristic evolution procedure that generates high-fidelity gravitational waveforms at I+ from numerical relativity simulations. Cauchy-characteristic evolution combines an interior solution of the Einstein field equations based on Cauchy slices with an exterior solution based on null slices that extend to I+. The foundation of our improved algorithm is a comprehensive method of handling the gauge transformations between the arbitrarily specified coordinates of the interior Cauchy evolution and the unique (up to Bondi-Metzner-Sachs group transformations) Bondi-Sachs coordinate system of the exterior characteristic evolution. We present a reformulated set of characteristic evolution equations better adapted to numerical implementation. In addition, we develop a method to ensure that the angular coordinates used in the volume during the characteristic evolution are asymptotically inertial. This provides a direct route to an expanded set of waveform outputs and is guaranteed to avoid pure-gauge logarithmic dependence that has caused trouble for previous spectral implementations of the characteristic evolution equations. We construct a set of Weyl scalars compatible with the Bondi-like coordinate systems used in characteristic evolution and determine simple, easily implemented forms for the asymptotic Weyl scalars in our suggested set of coordinates.", "date": "2020-08-15", "date_type": "published", "publication": "Physical Review D", "volume": "102", "number": "4", "publisher": "American Physical Society", "pagerange": "Art. No. 044052", "id_number": "CaltechAUTHORS:20200901-092407906", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200901-092407906", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Sherman Fairchild Foundation" }, { "agency": "NSF", "grant_number": "PHY-1708212" }, { "agency": "NSF", "grant_number": "PHY-1708213" }, { "agency": "NSF", "grant_number": "OAC-1931266" }, { "agency": "NSF", "grant_number": "PHY-1912081" }, { "agency": "NSF", "grant_number": "OAC-1931280" } ] }, "local_group": { "items": [ { "id": "TAPIR" }, { "id": "Walter-Burke-Institute-for-Theoretical-Physics" }, { "id": "Astronomy-Department" } ] }, "doi": "10.1103/physrevd.102.044052", "primary_object": { "basename": "2007.01339.pdf", "url": "https://authors.library.caltech.edu/records/xzcne-vwg56/files/2007.01339.pdf" }, "related_objects": [ { "basename": "PhysRevD.102.044052.pdf", "url": "https://authors.library.caltech.edu/records/xzcne-vwg56/files/PhysRevD.102.044052.pdf" } ], "resource_type": "article", "pub_year": "2020", "author_list": "Moxon, Jordan; Scheel, Mark A.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/hvje2-33765", "eprint_id": 103075, "eprint_status": "archive", "datestamp": "2023-08-19 21:27:40", "lastmod": "2023-10-20 00:45:23", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Okounkova-Maria", "name": { "family": "Okounkova", "given": "Maria" }, "orcid": "0000-0001-7869-5496" }, { "id": "Stein-L-C", "name": { "family": "Stein", "given": "Leo C." }, "orcid": "0000-0001-7559-9597" }, { "id": "Moxon-J", "name": { "family": "Moxon", "given": "Jordan" } }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Numerical relativity simulation of GW150914 beyond general relativity", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2020 American Physical Society. \n\nReceived 15 November 2019; accepted 15 April 2020; published 7 May 2020. \n\nWe thank Vijay Varma for computing the mismatch in Sec. III\u2009C. We thank Katerina Chatziioannou, Chad Galley, Francois Hebert for helpful discussions. We thank Dante Iozzo for useful comments on this manuscript. This work was supported in part by the Sherman Fairchild Foundation, and NSF Grants No. PHY-1708212 and No. PHY-1708213 at Caltech and No. PHY-1606654 at Cornell. The Flatiron Institute is supported by the Simons Foundation. L.\u2009C.\u2009S. acknowledges support from Award No. 80NSSC19M0053 to the MS NASA EPSCoR RID Program. All computations were performed on the Wheeler cluster at Caltech, which is supported by the Sherman Fairchild Foundation and by Caltech. All simulations are performed using the Spectral Einstein Code (SpEC) [45].\n\nPublished - PhysRevD.101.104016.pdf
Submitted - 1911.02588.pdf
", "abstract": "We produce the first astrophysically relevant numerical binary black hole gravitational waveform in a higher-curvature theory of gravity beyond general relativity. We simulate a system with parameters consistent with GW150914, the first LIGO detection, in order-reduced dynamical Chern-Simons gravity, a theory with motivations in string theory and loop quantum gravity. We present results for the leading-order corrections to the merger and ringdown waveforms, as well as the ringdown quasinormal mode spectrum. We estimate that such corrections may be discriminated in detections with signal to noise ratio \u2273180\u2013240, with the precise value depending on the dimension of the GR waveform family used in data analysis.", "date": "2020-05-15", "date_type": "published", "publication": "Physical Review D", "volume": "101", "number": "10", "publisher": "American Physical Society", "pagerange": "Art. No. 104016", "id_number": "CaltechAUTHORS:20200507-131200040", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200507-131200040", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Sherman Fairchild Foundation" }, { "agency": "NSF", "grant_number": "PHY-1708212" }, { "agency": "NSF", "grant_number": "PHY-1708213" }, { "agency": "NSF", "grant_number": "PHY-1606654" }, { "agency": "Simons Foundation" }, { "agency": "NASA", "grant_number": "80NSSC19M0053" } ] }, "local_group": { "items": [ { "id": "TAPIR" }, { "id": "Walter-Burke-Institute-for-Theoretical-Physics" }, { "id": "Astronomy-Department" } ] }, "doi": "10.1103/PhysRevD.101.104016", "primary_object": { "basename": "1911.02588.pdf", "url": "https://authors.library.caltech.edu/records/hvje2-33765/files/1911.02588.pdf" }, "related_objects": [ { "basename": "PhysRevD.101.104016.pdf", "url": "https://authors.library.caltech.edu/records/hvje2-33765/files/PhysRevD.101.104016.pdf" } ], "resource_type": "article", "pub_year": "2020", "author_list": "Okounkova, Maria; Stein, Leo C.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/y87cf-p6b57", "eprint_id": 98575, "eprint_status": "archive", "datestamp": "2023-08-19 18:53:55", "lastmod": "2023-10-18 17:28:42", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Giesler-M-D", "name": { "family": "Giesler", "given": "Matthew" }, "orcid": "0000-0003-2300-893X" }, { "id": "Isi-M", "name": { "family": "Isi", "given": "Maximiliano" }, "orcid": "0000-0001-8830-8672" }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Black hole ringdown: the importance of overtones", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2019 Published by the American Physical Society under the terms of the Creative Commons Attribution 4.0 International license. Further distribution of this work must maintain attribution to the author(s) and the published article's title, journal citation, and DOI. \n\nReceived 13 April 2019; revised manuscript received 14 August 2019; published 23 December 2019. \n\nThe authors thank Vijay Varma for many valuable discussions. We also thank Katerina Chatziioannou and Leo Stein for useful comments. M.\u2009G. and M.\u2009S. are supported by the Sherman Fairchild Foundation and NSF Grants No. PHY-1708212 and No. PHY-1708213 at Caltech. M.\u2009I. is a member of the LIGO Laboratory. LIGO was constructed by the California Institute of Technology and Massachusetts Institute of Technology with funding from the National Science Foundation and operates under Cooperative Agreement No. PHY-0757058. M.\u2009I. is supported by NASA through the NASA Hubble Fellowship Grant No. HST-HF2-51410.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under Contract No. NAS5-26555. S.\u2009T. is supported in part by the Sherman Fairchild Foundation and by NSF Grants No. PHY-1606654 and No. ACI-1713678 at Cornell. Computations were performed on the Wheeler cluster at Caltech, which is supported by the Sherman Fairchild Foundation and by Caltech. Computations were also performed on the Nemo computing cluster at the University of Wisconsin-Milwaukee, supported by NSF Grant No. PHY-1626190.\n\nPublished - PhysRevX.9.041060.pdf
Submitted - 1903.08284.pdf
", "abstract": "It is possible to infer the mass and spin of the remnant black hole from binary black hole mergers by comparing the ringdown gravitational wave signal to results from studies of perturbed Kerr spacetimes. Typically, these studies are based on the fundamental quasinormal mode of the dominant \u2113=m=2 harmonic. By modeling the ringdown of accurate numerical relativity simulations, we find, in agreement with previous findings, that the fundamental mode alone is insufficient to recover the true underlying mass and spin, unless the analysis is started very late in the ringdown. Including higher overtones associated with this \u2113=m=2 harmonic resolves this issue and provides an unbiased estimate of the true remnant parameters. Further, including overtones allows for the modeling of the ringdown signal for all times beyond the peak strain amplitude, indicating that the linear quasinormal regime starts much sooner than previously expected. This result implies that the spacetime is well described as a linearly perturbed black hole with a fixed mass and spin as early as the peak. A model for the ringdown beginning at the peak strain amplitude can exploit the higher signal-to-noise ratio in detectors, reducing uncertainties in the extracted remnant quantities. These results should be taken into consideration when testing the no-hair theorem.", "date": "2019-12", "date_type": "published", "publication": "Physical Review X", "volume": "9", "number": "4", "publisher": "American Physical Society", "pagerange": "Art. No. 041060", "id_number": "CaltechAUTHORS:20190911-124456116", "issn": "2160-3308", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190911-124456116", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Sherman Fairchild Foundation" }, { "agency": "NSF", "grant_number": "PHY-1708212" }, { "agency": "NSF", "grant_number": "PHY-1708213" }, { "agency": "NSF", "grant_number": "PHY-0757058" }, { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF2-51410.001-A" }, { "agency": "NASA", "grant_number": "NAS5-26555" }, { "agency": "NSF", "grant_number": "PHY-1606654" }, { "agency": "NSF", "grant_number": "ACI-1713678" }, { "agency": "NSF", "grant_number": "PHY-1626190" } ] }, "other_numbering_system": { "items": [ { "id": "P1900076", "name": "LIGO Document" } ] }, "local_group": { "items": [ { "id": "LIGO" }, { "id": "TAPIR" }, { "id": "Walter-Burke-Institute-for-Theoretical-Physics" }, { "id": "Astronomy-Department" } ] }, "doi": "10.1103/PhysRevX.9.041060", "primary_object": { "basename": "1903.08284.pdf", "url": "https://authors.library.caltech.edu/records/y87cf-p6b57/files/1903.08284.pdf" }, "related_objects": [ { "basename": "PhysRevX.9.041060.pdf", "url": "https://authors.library.caltech.edu/records/y87cf-p6b57/files/PhysRevX.9.041060.pdf" } ], "resource_type": "article", "pub_year": "2019", "author_list": "Giesler, Matthew; Isi, Maximiliano; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/nsg47-f1t91", "eprint_id": 98088, "eprint_status": "archive", "datestamp": "2023-08-19 18:44:24", "lastmod": "2023-10-18 17:02:00", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Okounkova-Maria", "name": { "family": "Okounkova", "given": "Maria" }, "orcid": "0000-0001-7869-5496" }, { "id": "Stein-L-C", "name": { "family": "Stein", "given": "Leo C." }, "orcid": "0000-0001-7559-9597" }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Numerical binary black hole collisions in dynamical Chern-Simons gravity", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2019 American Physical Society. \n\nReceived 20 June 2019; published 13 November 2019. \n\nThis work was supported in part by the Sherman Fairchild Foundation, and NSF Grants No. PHY-1708212 and No. PHY-1708213 at Caltech and No. PHY-1606654 at Cornell. Computations were performed using the Spectral Einstein Code [21]. All computations were performed on the Wheeler cluster at Caltech, which is supported by the Sherman Fairchild Foundation and by Caltech.\n\nPublished - PhysRevD.100.104026.pdf
Submitted - 1906.08789.pdf
", "abstract": "We produce the first numerical relativity binary black hole gravitational waveforms in a higher-curvature theory beyond general relativity. In particular, we study head-on collisions of binary black holes in order-reduced dynamical Chern-Simons gravity. This is a precursor to producing beyond-general-relativity waveforms for inspiraling binary black hole systems that are useful for gravitational wave detection. Head-on collisions are interesting in their own right, however, as they cleanly probe the quasinormal mode spectrum of the final black hole. We thus compute the leading-order dynamical Chern-Simons modifications to the complex frequencies of the postmerger gravitational radiation. We consider equal-mass systems, with equal spins oriented along the axis of collision, resulting in remnant black holes with spin. We find modifications to the complex frequencies of the quasinormal mode spectrum that behave as a power law with the spin of the remnant, and that are not degenerate with the frequencies associated with a Kerr black hole of any mass and spin. We discuss these results in the context of testing general relativity with gravitational wave observations.", "date": "2019-11-15", "date_type": "published", "publication": "Physical Review D", "volume": "100", "number": "10", "publisher": "American Physical Society", "pagerange": "Art. No. 104026", "id_number": "CaltechAUTHORS:20190821-152122696", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190821-152122696", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Sherman Fairchild Foundation" }, { "agency": "NSF", "grant_number": "PHY-1708212" }, { "agency": "NSF", "grant_number": "PHY-1708213" }, { "agency": "NSF", "grant_number": "PHY-1606654" }, { "agency": "Caltech" } ] }, "local_group": { "items": [ { "id": "TAPIR" }, { "id": "Walter-Burke-Institute-for-Theoretical-Physics" }, { "id": "Astronomy-Department" } ] }, "doi": "10.1103/PhysRevD.100.104026", "primary_object": { "basename": "PhysRevD.100.104026.pdf", "url": "https://authors.library.caltech.edu/records/nsg47-f1t91/files/PhysRevD.100.104026.pdf" }, "related_objects": [ { "basename": "1906.08789.pdf", "url": "https://authors.library.caltech.edu/records/nsg47-f1t91/files/1906.08789.pdf" } ], "resource_type": "article", "pub_year": "2019", "author_list": "Okounkova, Maria; Stein, Leo C.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/w4v51-btm03", "eprint_id": 98090, "eprint_status": "archive", "datestamp": "2023-08-19 18:44:31", "lastmod": "2023-10-18 17:02:06", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Chatziioannou-K", "name": { "family": "Chatziioannou", "given": "Katerina" }, "orcid": "0000-0002-5833-413X" }, { "id": "Barkett-Kevin", "name": { "family": "Barkett", "given": "Kevin" }, "orcid": "0000-0001-8230-4363" }, { "id": "Blackman-Jonathan", "name": { "family": "Blackman", "given": "Jonathan" }, "orcid": "0000-0002-7113-0289" }, { "id": "Giesler-Matthew-D", "name": { "family": "Giesler", "given": "Matthew" }, "orcid": "0000-0003-2300-893X" }, { "id": "Hemberger-Daniel-A", "name": { "family": "Hemberger", "given": "Daniel" } }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." }, "orcid": "0000-0001-6656-9134" }, { "id": "Szil\u00e1gyi-B\u00e9la", "name": { "family": "Szil\u00e1gyi", "given": "B\u00e9la" }, "orcid": "0000-0001-7744-6180" }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "On the properties of the massive binary black hole merger GW170729", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2019 American Physical Society.\n\nReceived 18 March 2019; published 7 November 2019.\n\nWe thank Christopher Berry, Thomas Dent, Tristano DiGirolamo, Bhooshan Gadre, Roland Haas, Nathan Johnson-McDaniel, Riccardo Sturani, and Aaron Zimmerman for helpful comments and suggestions. This research has made use of data, software and/or web tools obtained from the Gravitational Wave Open Science Center (https://www.gw-openscience.org), a service of LIGO Laboratory, the LIGO Scientific Collaboration and the Virgo Collaboration. LIGO is funded by the U.S. National Science Foundation. Virgo is funded by the French Centre National de Recherche Scientifique (CNRS), the Italian Istituto Nazionale della Fisica Nucleare (INFN) and the Dutch Nikhef, with contributions by Polish and Hungarian institutes. The Flatiron Institute is supported by the Simons Foundation. J.\u2009C.\u2009B. acknowledges support from Australian Research Council Discovery Project DP180103155. C.\u2009J.\u2009H, K.\u2009K.\u2009Y.\u2009N and S.\u2009V. acknowledges the support of the National Science Foundation and the LIGO Laboratory. LIGO was constructed by the California Institute of Technology and Massachusetts Institute of Technology with funding from the National Science Foundation and operates under cooperative agreement PHY-1764464. M.\u2009H. was supported by Science and Technology Facilities Council (STFC) Grant No. ST/L000962/1 and European Research Council Consolidator Grant No. 647839. Parts of this research were conducted by the Australian Research Council Centre of Excellence for Gravitational Wave Discovery (OzGrav), through Project No. CE170100004. R.\u2009O.\u2009S. and J.\u2009L. are supported by National Science Foundation (NSF) Grants No. PHY-1707965 and No. PHY-1607520. P.\u2009S. acknowledges support from the NWO Veni grant no. 680-47-460 and the Science and Technology Facilities Council Grant No. ST/N000633/1. M.\u2009H. acknowledges support from the Swiss National Science Foundation (SNSF) Grant No. IZCOZ0_177057. L.\u2009S. was supported by the Young Elite Scientists Sponsorship Program by the China Association for Science and Technology (2018QNRC001), and partially supported by the National Science Foundation of China (11721303), and XDB23010200. The GT authors gratefully acknowledge the NSF for financial support from Grants No. PHY 1806580, No. PHY 1809572, and No. TG-PHY120016. Computational resources were provided by XSEDE and the Georgia Tech Cygnus Cluster. The RIT authors gratefully acknowledge the NSF for financial support from Grants No. PHY-1607520, No. PHY-1707946, No. ACI-1550436, No. AST-1516150, No. ACI-1516125, No. PHY-1726215. This work used the Extreme Science and Engineering Discovery Environment (XSEDE) [allocation TG-PHY060027N], which is supported by NSF grant No. ACI-1548562. Computational resources were also provided by the NewHorizons, BlueSky Clusters, and Green Prairies at the Rochester Institute of Technology, which were supported by NSF grants No. PHY-0722703, No. DMS-0820923, No. AST-1028087, No. PHY-1229173, and No. PHY-1726215. The SXS authors at Caltech acknowledge the Sherman Fairchild Foundation, and NSF Grants No. PHY-1708212 and No. PHY-1708213. G.\u2009L., N.\u2009A., and A.\u2009G. are supported by NSF Grants No. PHY-1606522, No. PHY-1654359, No. PHY-1654359. Computations were done using the orca cluster supported in part by PHY-1429873 and by Cal State Fullerton. A.\u2009G. is also supported in part by Nancy Goodhue-McWilliams. The authors are grateful for computational resources provided by the LIGO Laboratory and supported by National Science Foundation Grants No. PHY-0757058 and No. PHY-0823459. Some of the computational work for this manuscript was also carried out on the computer cluster vULCAN at the Max Planck Institute for Gravitational Physics in Potsdam. Plots have been made with matplotlib [107] and corner [108].\n\nPublished - PhysRevD.100.104015.pdf
Submitted - 1903.06742.pdf
", "abstract": "We present a detailed investigation into the properties of GW170729, the gravitational wave with the most massive and distant source confirmed to date. We employ an extensive set of waveform models, including new improved models that incorporate the effect of higher-order waveform modes which are particularly important for massive systems. We find no indication of spin-precession, but the inclusion of higher-order modes in the models results in an improved estimate for the mass ratio of (0.3\u20130.8) at the 90% credible level. Our updated measurement excludes equal masses at that level. We also find that models with higher-order modes lead to the data being more consistent with a smaller effective spin, with the probability that the effective spin is greater than zero being reduced from 99% to 94%. The 90% credible interval for the effective spin parameter is now (\u22120.01\u22120.50). Additionally, the recovered signal-to-noise ratio increases by \u223c0.3 units compared to analyses without higher-order modes; the overall Bayes factor in favor of the presence of higher-order modes in the data is 5.1\u22361. We study the effect of common spin priors on the derived spin and mass measurements, and observe small shifts in the spins, while the masses remain unaffected. We argue that our conclusions are robust against systematic errors in the waveform models. We also compare the above waveform-based analysis which employs compact-binary waveform models to a more flexible wavelet- and chirplet-based analysis. We find consistency between the two, with overlaps of \u223c0.9, typical of what is expected from simulations of signals similar to GW170729, confirming that the data are well-described by the existing waveform models. Finally, we study the possibility that the primary component of GW170729 was the remnant of a past merger of two black holes and find this scenario to be indistinguishable from the standard formation scenario.", "date": "2019-11-15", "date_type": "published", "publication": "Physical Review D", "volume": "100", "number": "10", "publisher": "American Physical Society", "pagerange": "Art. No. 104015", "id_number": "CaltechAUTHORS:20190821-153756552", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190821-153756552", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Centre National de Recherche Scientifique (CNRS)" }, { "agency": "Istituto Nazionale di Fisica Nucleare (INFN)" }, { "agency": "Nikhef" }, { "agency": "Australian Research Council", "grant_number": "DP180103155" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/L000962/1" }, { "agency": "European Research Council (ERC)", "grant_number": "647839" }, { "agency": "Australian Research Council", "grant_number": "CE170100004" }, { "agency": "NSF", "grant_number": "PHY-1707965" }, { "agency": "NSF", "grant_number": "PHY-1607520" }, { "agency": "Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)", "grant_number": "680-47-460" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/N000633/1" }, { "agency": "Swiss National Science Foundation (SNSF)", "grant_number": "IZCOZ0 177057" }, { "agency": "China Association for Science and Technology", "grant_number": "2018QNRC001" }, { "agency": "National Natural Science Foundation of China", "grant_number": "11721303" }, { "agency": "National Natural Science Foundation of China", "grant_number": "XDB23010200" }, { "agency": "NSF", "grant_number": "PHY-1806580" }, { "agency": "NSF", "grant_number": "PHY-1809572" }, { "agency": "NSF", "grant_number": "TG-PHY120016" }, { "agency": "NSF", "grant_number": "PHY-1607520" }, { "agency": "NSF", "grant_number": "PHY-1707946" }, { "agency": "NSF", "grant_number": "ACI- 1550436" }, { "agency": "NSF", "grant_number": "AST-1516150" }, { "agency": "NSF", "grant_number": "ACI-1516125" }, { "agency": "NSF", "grant_number": "PHY-1726215" }, { "agency": "NSF", "grant_number": "TG-PHY060027N" }, { "agency": "NSF", "grant_number": "ACI-1548562" }, { "agency": "NSF", "grant_number": "PHY-0722703" }, { "agency": "NSF", "grant_number": "DMS-0820923" }, { "agency": "NSF", "grant_number": "AST-1028087" }, { "agency": "NSF", "grant_number": "PHY-1229173" }, { "agency": "Sherman Fairchild Foundation" }, { "agency": "NSF", "grant_number": "PHY-1708212" }, { "agency": "NSF", "grant_number": "PHY-1708213" }, { "agency": "NSF", "grant_number": "PHY-1606522" }, { "agency": "NSF", "grant_number": "PHY-1654359" }, { "agency": "NSF", "grant_number": "PHY-1429873" }, { "agency": "California State University, Fullerton" }, { "agency": "Nancy Goodhue-McWilliams" }, { "agency": "NSF", "grant_number": "PHY-0757058" }, { "agency": "NSF", "grant_number": "PHY-0823459" }, { "agency": "NSF", "grant_number": "PHY-1764464" } ] }, "local_group": { "items": [ { "id": "LIGO" }, { "id": "TAPIR" }, { "id": "Astronomy-Department" } ] }, "doi": "10.1103/PhysRevD.100.104015", "primary_object": { "basename": "PhysRevD.100.104015.pdf", "url": "https://authors.library.caltech.edu/records/w4v51-btm03/files/PhysRevD.100.104015.pdf" }, "related_objects": [ { "basename": "1903.06742.pdf", "url": "https://authors.library.caltech.edu/records/w4v51-btm03/files/1903.06742.pdf" } ], "resource_type": "article", "pub_year": "2019", "author_list": "Chatziioannou, Katerina; Barkett, Kevin; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/td1d3-x4n84", "eprint_id": 95007, "eprint_status": "archive", "datestamp": "2023-08-19 18:16:03", "lastmod": "2023-10-20 18:29:04", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Boyle-Michael", "name": { "family": "Boyle", "given": "Michael" }, "orcid": "0000-0002-5075-5116" }, { "id": "Hemberger-Daniel-A", "name": { "family": "Hemberger", "given": "Daniel" } }, { "name": { "family": "Iozzo", "given": "Dante A. B." } }, { "name": { "family": "Lovelace", "given": "Geoffrey" }, "orcid": "0000-0002-7084-1070" }, { "name": { "family": "Ossokine", "given": "Serguei" }, "orcid": "0000-0002-2579-1246" }, { "name": { "family": "Pfeiffer", "given": "Harald P." }, "orcid": "0000-0001-9288-519X" }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." }, "orcid": "0000-0001-6656-9134" }, { "id": "Stein-Leo-C", "name": { "family": "Stein", "given": "Leo C." }, "orcid": "0000-0001-7559-9597" }, { "name": { "family": "Woodford", "given": "Charles J." }, "orcid": "0000-0003-4174-0577" }, { "name": { "family": "Zimmerman", "given": "Aaron B." } }, { "name": { "family": "Afshari", "given": "Nousha" } }, { "id": "Barkett-Kevin", "name": { "family": "Barkett", "given": "Kevin" }, "orcid": "0000-0001-8230-4363" }, { "id": "Blackman-Jonathan", "name": { "family": "Blackman", "given": "Jonathan" }, "orcid": "0000-0002-7113-0289" }, { "id": "Chatziioannou-K", "name": { "family": "Chatziioannou", "given": "Katerina" }, "orcid": "0000-0002-5833-413X" }, { "name": { "family": "Chu", "given": "Tony" } }, { "name": { "family": "Demos", "given": "Nicholas" } }, { "name": { "family": "Deppe", "given": "Nils" }, "orcid": "0000-0003-4557-4115" }, { "name": { "family": "Field", "given": "Scott E." } }, { "name": { "family": "Fischer", "given": "Nils L." } }, { "name": { "family": "Foley", "given": "Evan" } }, { "name": { "family": "Fong", "given": "Heather" } }, { "name": { "family": "Garcia", "given": "Alyssa" } }, { "id": "Giesler-Matthew-D", "name": { "family": "Giesler", "given": "Matthew" }, "orcid": "0000-0003-2300-893X" }, { "id": "H\u00e9bert-Fran\u00e7ois", "name": { "family": "H\u00e9bert", "given": "Fran\u00e7ois" }, "orcid": "0000-0001-9009-6955" }, { "name": { "family": "Hinder", "given": "Ian" }, "orcid": "0000-0003-3548-9101" }, { "name": { "family": "Katebi", "given": "Reza" } }, { "name": { "family": "Khan", "given": "Haroon" } }, { "name": { "family": "Kidder", "given": "Lawrence E." }, "orcid": "0000-0001-5392-7342" }, { "name": { "family": "Kumar", "given": "Prayush" } }, { "name": { "family": "Kuper", "given": "Kevin" } }, { "id": "Lim-Halston", "name": { "family": "Lim", "given": "Halston" } }, { "id": "Okounkova-Maria", "name": { "family": "Okounkova", "given": "Maria" }, "orcid": "0000-0001-7869-5496" }, { "name": { "family": "Ramirez", "given": "Teresita" } }, { "name": { "family": "Rodriguez", "given": "Samuel" } }, { "name": { "family": "R\u00fcter", "given": "Hannes R." } }, { "id": "Schmidt-Patricia", "name": { "family": "Schmidt", "given": "Patricia" } }, { "id": "Szil\u00e1gyi-B\u00e9la", "name": { "family": "Szil\u00e1gyi", "given": "B\u00e9la" }, "orcid": "0000-0001-7744-6180" }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" }, { "id": "Varma-Vijay", "name": { "family": "Varma", "given": "Vijay" }, "orcid": "0000-0002-9994-1761" }, { "id": "Walker-Marissa", "name": { "family": "Walker", "given": "Marissa" }, "orcid": "0000-0002-7176-6914" } ] }, "title": "The SXS Collaboration catalog of binary black hole simulations", "ispublished": "pub", "full_text_status": "public", "keywords": "numerical relativity, black holes, gravitational waves", "note": "\u00a9 2019 IOP Publishing Ltd. \n\nReceived 9 April 2019, revised 3 July 2019; Accepted for publication 24 July 2019; Published 11 September 2019. \n\nWe are pleased to thank Davide Gerosa and Josh Smith for helpful discussions. This work was supported in part by the Sherman Fairchild Foundation, NSF Grants PHY-1708212 and PHY-1708213 at Caltech, NSF Grants PHY-1606654 and DGE-1650441 at Cornell, NSF Grants PHY-1606522, PHY-1654359, and AST-1559694 and by Dan Black and Goodhue-McWilliams at Cal State Fullerton. S E Field is partially supported by NSF Grant PHY-1806665. H. Fong and C. J. Woodford acknowledge support from NSERC of Canada grant PGSD3-504366-2017, and H. Fong further acknowledges support from the University of Toronto and the Japan Society for the Promotion of Science. P. Schmidt acknowledges support from the NWO Veni Grant No. 680-47-460. This work used the Extreme Science and Engineering Discovery Environment (XSEDE), which is supported by National Science Foundation Grant No. ACI-1548562. This research is part of the Blue Waters sustained-petascale computing project, which is supported by the National Science Foundation (awards OCI-0725070 and ACI-1238993) and the state of Illinois. Blue Waters is a joint effort of the University of Illinois at Urbana-Champaign and its National Center for Supercomputing Applications. Computations were performed on the GPC supercomputer at the SciNet HPC Consortium [232]; SciNet is funded by: the Canada Foundation for Innovation (CFI) under the auspices of Compute Canada; the Government of Ontario; Ontario Research Fund (ORF)\u2014Research Excellence; and the University of Toronto. Computations were performed on the supercomputer Briare\u00e9 from the Universit\u00e9 de Montr\u00e9al, managed by Calcul Qu\u00e9bec and Compute Canada. The operation of these supercomputers is funded by the Canada Foundation for Innovation (CFI), NanoQu\u00e9bec, RMGA and the Fonds de recherche du Qu\u00e9bec-Nature et Technologie (FRQ-NT). Computations were performed on the Wheeler cluster at Caltech, which is supported by the Sherman Fairchild Foundation and by Caltech; on NSF/NCSA Blue Waters under allocation NSF PRAC\u20131713694; and on XSEDE resources Bridges at the Pittsburgh Supercomputing Center, Comet at the San Diego Supercomputer Center, and Stampede and Stampede2 at the Texas Advanced Computing Center, through allocation TG-PHY990007N. Computations were performed on the Minerva high-performance computer cluster at the Max Planck Institute for Gravitational Physics in Potsdam.\n\nSubmitted - 1904.04831.pdf
", "abstract": "Accurate models of gravitational waves from merging black holes are necessary for detectors to observe as many events as possible while extracting the maximum science. Near the time of merger, the gravitational waves from merging black holes can be computed only using numerical relativity. In this paper, we present a major update of the Simulating eXtreme Spacetimes (SXS) Collaboration catalog of numerical simulations for merging black holes. The catalog contains 2018 distinct configurations (a factor of 11 increase compared to the 2013 SXS catalog), including 1426 spin-precessing configurations, with mass ratios between 1 and 10, and spin magnitudes up to 0.998. The median length of a waveform in the catalog is 39 cycles of the dominant \u2113 = m = 2 gravitational-wave mode, with the shortest waveform containing 7.0 cycles and the longest 351.3 cycles. We discuss improvements such as correcting for moving centers of mass and extended coverage of the parameter space. We also present a thorough analysis of numerical errors, finding typical truncation errors corresponding to a waveform mismatch of\u2009\u2009~10\u22124. The simulations provide remnant masses and spins with uncertainties of 0.03% and 0.1% (90th percentile), about an order of magnitude better than analytical models for remnant properties. The full catalog is publicly available at www.black-holes.org/waveforms.", "date": "2019-10-10", "date_type": "published", "publication": "Classical and Quantum Gravity", "volume": "36", "number": "19", "publisher": "IOP", "pagerange": "Art. No. 195006", "id_number": "CaltechAUTHORS:20190426-082059591", "issn": "0264-9381", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190426-082059591", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY-1708212" }, { "agency": "NSF", "grant_number": "PHY-1708213" }, { "agency": "NSF", "grant_number": "PHY-1606654" }, { "agency": "NSF Graduate Research Fellowship", "grant_number": "DGE-1650441" }, { "agency": "NSF", "grant_number": "PHY-1606522" }, { "agency": "NSF", "grant_number": "PHY-1654359" }, { "agency": "NSF", "grant_number": "AST-1559694" }, { "agency": "NSF", "grant_number": "PHY-1806665" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)", "grant_number": "PGSD3-504366-2017" }, { "agency": "University of Toronto" }, { "agency": "Japan Society for the Promotion of Science (JSPS)" }, { "agency": "Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)", "grant_number": "680-47-460" }, { "agency": "NSF", "grant_number": "ACI-1548562" }, { "agency": "NSF", "grant_number": "OCI-0725070" }, { "agency": "NSF", "grant_number": "ACI-1238993" }, { "agency": "State of Illinois" }, { "agency": "Canada Foundation for Innovation" }, { "agency": "Compute Canada" }, { "agency": "Ontario Research Fund-Research Excellence" }, { "agency": "NanoQu\u00e9bec" }, { "agency": "RMGA" }, { "agency": "Fonds de recherche du Qu\u00e9be-Nature et technologies (FRQ-NT)" }, { "agency": "Sherman Fairchild Foundation" }, { "agency": "Caltech" }, { "agency": "NSF", "grant_number": "OAC-1713694" }, { "agency": "NSF", "grant_number": "TG-PHY990007N" } ] }, "local_group": { "items": [ { "id": "TAPIR" }, { "id": "Astronomy-Department" } ] }, "doi": "10.1088/1361-6382/ab34e2", "primary_object": { "basename": "1904.04831.pdf", "url": "https://authors.library.caltech.edu/records/td1d3-x4n84/files/1904.04831.pdf" }, "resource_type": "article", "pub_year": "2019", "author_list": "Boyle, Michael; Hemberger, Daniel; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/fdvbe-gq464", "eprint_id": 99015, "eprint_status": "archive", "datestamp": "2023-08-19 17:53:15", "lastmod": "2023-10-18 17:47:41", "type": "monograph", "metadata_visibility": "show", "creators": { "items": [ { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" }, { "id": "Vallisneri-Michele", "name": { "family": "Vallisneri", "given": "Michele" }, "orcid": "0000-0002-4162-0033" }, { "id": "Chua-Alvin-J-K", "name": { "family": "Chua", "given": "Alvin" }, "orcid": "0000-0001-5242-8269" }, { "id": "Akeson-Rachel-L", "name": { "family": "Akeson", "given": "Rachel" }, "orcid": "0000-0001-9674-1564" }, { "id": "Archibald-Anne-M", "name": { "family": "Archibald", "given": "Anne M." }, "orcid": "0000-0003-0638-3340" }, { "id": "Babak-Stanislav", "name": { "family": "Babak", "given": "Stanislav" }, "orcid": "0000-0001-7469-4250" }, { "id": "Breivik-Katelyn", "name": { "family": "Breivik", "given": "Katelyn" }, "orcid": "0000-0001-5228-6598" }, { "id": "Brown-C-Titus", "name": { "family": "Brown", "given": "C. Titus" }, "orcid": "0000-0001-6001-2677" }, { "id": "Cornish-Neil-J", "name": { "family": "Cornish", "given": "Neil J." }, "orcid": "0000-0002-7435-0869" }, { "id": "Cutler-Curt-J", "name": { "family": "Cutler", "given": "Curt J." }, "orcid": "0000-0002-2080-1468" }, { "id": "Davidoff-Scott", "name": { "family": "Davidoff", "given": "Scott" }, "orcid": "0000-0002-4417-7268" }, { "id": "Foucart-Fran\u00e7ois", "name": { "family": "Foucart", "given": "Francois" }, "orcid": "0000-0003-4617-4738" }, { "id": "Galley-Chad-R", "name": { "family": "Galley", "given": "Chad R." } }, { "id": "Kidder-Lawrence-E", "name": { "family": "Kidder", "given": "Lawrence E." }, "orcid": "0000-0001-5392-7342" }, { "id": "Kumar-Prayush", "name": { "family": "Kumar", "given": "Prayush" }, "orcid": "0000-0001-5523-4603" }, { "id": "Lamberts-Astrid", "name": { "family": "Lamberts", "given": "Astrid" }, "orcid": "0000-0001-8740-0127" }, { "id": "Lovelace-Geoffrey", "name": { "family": "Lovelace", "given": "Geoffrey" }, "orcid": "0000-0002-7084-1070" }, { "id": "Mahabal-Ashish-A", "name": { "family": "Mahabal", "given": "Ashish" }, "orcid": "0000-0003-2242-0244" }, { "id": "Moran-Christine-C", "name": { "family": "Moran", "given": "Christine Corbett" }, "orcid": "0000-0003-2088-7465" }, { "id": "Nuttall-Laura-K", "name": { "family": "Nuttall", "given": "Laura" }, "orcid": "0000-0002-8599-8791" }, { "id": "Okounkova-Maria", "name": { "family": "Okounkova", "given": "Maria" }, "orcid": "0000-0001-7869-5496" }, { "id": "Robson-Travis", "name": { "family": "Robson", "given": "Travis" }, "orcid": "0000-0001-9076-5055" }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." }, "orcid": "0000-0001-6656-9134" }, { "id": "Shoemaker-Deridre-M", "name": { "family": "Shoemaker", "given": "Deirdre" } }, { "id": "Taylor-Stephen-R", "name": { "family": "Taylor", "given": "Stephen" }, "orcid": "0000-0003-0264-1453" }, { "id": "Tinto-Massimo", "name": { "family": "Tinto", "given": "Massimo" }, "orcid": "0000-0002-8107-5148" }, { "id": "Varma-Vijay", "name": { "family": "Varma", "given": "Vijay" }, "orcid": "0000-0002-9994-1761" }, { "id": "Vecchio-Alberto", "name": { "family": "Vecchio", "given": "Alberto" }, "orcid": "0000-0002-6254-1617" } ] }, "title": "The Architecture of the LISA Science Analysis", "ispublished": "unpub", "full_text_status": "public", "note": "\u00a9 September 2019. \n\nThis work had its inception at the Architecture of the LISA Science Analysis study funded by the W. M. Keck Institute for Space Studies. The study organizers and all study participants are deeply grateful to KISS Executive Director Michele Judd and to her amazing staff for creating the perfect environment for insight, creativity, and collegiality. Deirdre Shoemaker acknowledges support from NSF award PHY1806580. Michele Vallisneri, Alvin Chua, Curt Cutler, and Chad Galley acknowledge support from the JPL RTD program. Part of this work was performed at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Government sponsorship acknowledged.\n\nAccepted Version - LISA_Final_Report.pdf
", "abstract": "The space-based gravitational-wave (henceforth, GW!) observatory LISA (Amaro-Seoane et al., 2017) will o\u02d9er unparalleled science returns, including a view of massive black hole mergers up to high redshifts, precision tests of general relativity and black hole structure, a census of thousands of compact binaries in the Galaxy, and the possibility of detecting stochastic signals from the early Universe.\nWhile the Mock LISA Data Challenges (2006\u20132011) gave us confidence that LISA will be able to fulfill its scientific potential, we still have a rather incomplete idea of what the end-to-end LISA science analysis should look like. The task at hand is substantial:\n1) Our data reduction process needs to ensure the phase coherence of GW measurements across data gaps and instrument glitches over multiple years.\n2) Our waveform models need to reach part-in-105 accuracy to maximize the science payo\u02d9 of the mission, with su\u00ffcient computational e\u00ffciency to sample parameter space broadly.\n3) Our algorithms need to resolve thousands of individual sources of di\u02d9erent types and strengths, all of them superimposed on the same multi-year dataset, while simultaneously characterizing the underlying noise-like stochastic background.\n4) Our catalogs need to represent the complex and high-dimensional joint distributions of estimated source parameters for all sources.\nIt is tempting to assume that current algorithms and prototype codes will scale up to this challenge, thanks to the greatly increased computational power that will become available by the time of LISA's launch in the early 2030s. In reality, harnessing that power will require very di\u02d9erent methods, adapted to future high-performance computational architectures that we can only glimpse now. Thus, we need to begin our exploration at this time, seeking inspiration from other disciplines (e.g., big data processing, computational biology, the most advanced applications in astroinformatics) and learning to pose the same physical questions in di\u02d9erent, future-proof ways\u2014or even daring to imagine questions that will be tractable only with future machines.\nThe broad objective of this study was to imagine how evolved or rethought data analysis algorithms and source-modeling codes will perform the LISA science analysis on the computers of the future, with the hope of guiding LISA science and data analysis research and development in the years to come.", "date": "2019-10-03", "date_type": "published", "id_number": "CaltechAUTHORS:20191002-102632020", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20191002-102632020", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Keck Institute for Space Studies (KISS)" }, { "agency": "NSF", "grant_number": "PHY-1806580" }, { "agency": "JPL Research and Technology Development Fund" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Keck-Institute-for-Space-Studies" }, { "id": "Astronomy-Department" } ] }, "doi": "10.26206/NTBV-YA50", "primary_object": { "basename": "LISA_Final_Report.pdf", "url": "https://authors.library.caltech.edu/records/fdvbe-gq464/files/LISA_Final_Report.pdf" }, "resource_type": "monograph", "pub_year": "2019", "author_list": "Teukolsky, Saul A.; Vallisneri, Michele; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/mg8b7-8mk09", "eprint_id": 98713, "eprint_status": "archive", "datestamp": "2023-08-19 00:58:12", "lastmod": "2023-10-18 17:35:27", "type": "monograph", "metadata_visibility": "show", "creators": { "items": [ { "id": "Baumgarte-T-W", "name": { "family": "Baumgarte", "given": "T. W." } }, { "id": "Shapiro-S-L", "name": { "family": "Shapiro", "given": "S. L." } }, { "id": "Cook-G-B", "name": { "family": "Cook", "given": "G. B." } }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "M. A." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "S. A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Binary Neutron Stars in Quasi-Equilibrium Circular Orbit: A Fully Relativistic Treatment", "ispublished": "unpub", "full_text_status": "public", "note": "Submitted - 9701033.pdf
", "abstract": "We present a numerical scheme that solves the initial value problem in full general relativity for a binary neutron star in quasi-equilibrium. While Newtonian gravity allows for a strict equilibrium, a relativistic binary system emits gravitational radiation, causing the system to lose energy and slowly spiral inwards. However, since inspiral occurs on a time scale much longer than the orbital period, we can adopt a quasi-equilibrium approximation. In this approximation, we integrate a subset of the Einstein equations coupled to the equations of relativistic hydrodynamics to solve the initial value problem for binaries of arbitrary separation, down to the innermost stable orbit.", "date": "2019-09-18", "date_type": "published", "id_number": "CaltechAUTHORS:20190918-094403809", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190918-094403809", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "doi": "10.48550/arXiv.9701033", "primary_object": { "basename": "9701033.pdf", "url": "https://authors.library.caltech.edu/records/mg8b7-8mk09/files/9701033.pdf" }, "resource_type": "monograph", "pub_year": "2019", "author_list": "Baumgarte, T. W.; Shapiro, S. L.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/c9w8g-p1z36", "eprint_id": 98089, "eprint_status": "archive", "datestamp": "2023-08-19 17:51:18", "lastmod": "2023-10-18 17:02:03", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Isi-M", "name": { "family": "Isi", "given": "Maximiliano" }, "orcid": "0000-0001-8830-8672" }, { "id": "Giesler-M-D", "name": { "family": "Giesler", "given": "Matthew" }, "orcid": "0000-0003-2300-893X" }, { "id": "Farr-W-M", "name": { "family": "Farr", "given": "Will M." }, "orcid": "0000-0003-1540-8562" }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Testing the no-hair theorem with GW150914", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2019 American Physical Society. \n\nReceived 5 May 2019; published 12 September 2019. \n\nThis research has made use of data, software, and/or Web tools obtained from the Gravitational Wave Open Science Center [50,56], a service of the LIGO Laboratory, the LIGO Scientific Collaboration, and the Virgo Collaboration. \n\nWe thank Aaron Zimmerman for valuable feedback. We thank Gregorio Carullo, Walter del Pozzo, and John Veitch for discussions of their paper on and methods for time-domain analysis [29]. We thank Alessandra Buonanno for clarifications on past use of quasinormal and pseudoquasinormal ringdown modes in waveform modeling. M. I. is supported by NASA through the NASA Hubble Fellowship Grant No. HST-HF2-51410.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under Contract No. NAS5-26555. M. I. is a member of the LIGO Laboratory. LIGO was constructed by the California Institute of Technology and Massachusetts Institute of Technology with funding from the National Science Foundation and operates under Cooperative Agreement No. PHY-0757058. M. G. and M. A. S. are supported by the Sherman Fairchild Foundation and NSF Grants No. PHY-1708212 and No. PHY-1708213 at Caltech. S. A. T. is supported in part by the Sherman Fairchild Foundation and by NSF Grants No. PHY-1606654 and No. ACI-1713678 at Cornell. The Flatiron Institute is supported by the Simons Foundation. This paper carries LIGO Document No. LIGO-P1900135.\n\nPublished - PhysRevLett.123.111102.pdf
Submitted - 1905.00869.pdf
", "abstract": "We analyze gravitational-wave data from the first LIGO detection of a binary black-hole merger (GW150914) in search of the ringdown of the remnant black hole. Using observations beginning at the peak of the signal, we find evidence of the fundamental quasinormal mode and at least one overtone, both associated with the dominant angular mode (\u2113=m=2), with 3.6\u03c3 confidence. A ringdown model including overtones allows us to measure the final mass and spin magnitude of the remnant exclusively from postinspiral data, obtaining an estimate in agreement with the values inferred from the full signal. The mass and spin values we measure from the ringdown agree with those obtained using solely the fundamental mode at a later time, but have smaller uncertainties. Agreement between the postinspiral measurements of mass and spin and those using the full waveform supports the hypothesis that the GW150914 merger produced a Kerr black hole, as predicted by general relativity, and provides a test of the no-hair theorem at the \u223c10% level. An independent measurement of the frequency of the first overtone yields agreement with the no-hair hypothesis at the \u223c20% level. As the detector sensitivity improves and the detected population of black hole mergers grows, we can expect that using overtones will provide even stronger tests.", "date": "2019-09-13", "date_type": "published", "publication": "Physical Review Letters", "volume": "123", "number": "11", "publisher": "American Physical Society", "pagerange": "Art. No. 111102", "id_number": "CaltechAUTHORS:20190821-152942401", "issn": "0031-9007", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190821-152942401", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF2-51410.001-A" }, { "agency": "NASA", "grant_number": "NAS5-26555" }, { "agency": "NSF", "grant_number": "PHY-0757058" }, { "agency": "Sherman Fairchild Foundation" }, { "agency": "NSF", "grant_number": "PHY-1708212" }, { "agency": "NSF", "grant_number": "PHY-1708213" }, { "agency": "NSF", "grant_number": "PHY-1606654" }, { "agency": "NSF", "grant_number": "ACI-1713678" }, { "agency": "Simons Foundation" } ] }, "other_numbering_system": { "items": [ { "id": "P1900135", "name": "LIGO Document" } ] }, "local_group": { "items": [ { "id": "LIGO" }, { "id": "TAPIR" }, { "id": "Walter-Burke-Institute-for-Theoretical-Physics" }, { "id": "Astronomy-Department" } ] }, "doi": "10.1103/PhysRevLett.123.111102", "primary_object": { "basename": "1905.00869.pdf", "url": "https://authors.library.caltech.edu/records/c9w8g-p1z36/files/1905.00869.pdf" }, "related_objects": [ { "basename": "PhysRevLett.123.111102.pdf", "url": "https://authors.library.caltech.edu/records/c9w8g-p1z36/files/PhysRevLett.123.111102.pdf" } ], "resource_type": "article", "pub_year": "2019", "author_list": "Isi, Maximiliano; Giesler, Matthew; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/d6xq5-sx695", "eprint_id": 98318, "eprint_status": "archive", "datestamp": "2023-08-19 04:58:16", "lastmod": "2023-10-18 17:15:11", "type": "monograph", "metadata_visibility": "show", "creators": { "items": [ { "id": "Landry-Walter", "name": { "family": "Landry", "given": "Walter" } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "An Efficient Method for Fully Relativistic Simulations of Coalescing Binary Neutron Stars", "ispublished": "unpub", "full_text_status": "public", "note": "We wish to thank Mark Scheel, Greg Cook and Larry Kidder for many useful discussions. We would also like to thank Mark Miller for answering questions about his numerical relativity code, Scott Baden for his help with getting Kelp to work, Roger Lovelace for his help with hydrodynamics, and Thomas Baumgarte for his help with outer boundary conditions. This work was supported in part by NSF grants PHY 98-00737 and 99-00672, and NASA Grant NAG5-7264 to Cornell University.\n\nSubmitted - 9912004.pdf
", "abstract": "The merger of two neutron stars has been proposed as a source of gamma-ray bursts, r-process elements, and detectable gravitational waves. Extracting information from observations of these phenomena requires fully relativistic simulations. Unfortunately, the only demonstrated method for stably evolving neutron stars requires solving elliptic equations at each time step, adding substantially to the computational resources required. In this paper we present a simpler, more efficient method. The key insight is in how we apply numerical diffusion. We perform a number of tests to validate the method and our implementation. We also carry out a very rough simulation of coalescence and extraction of the gravitational waves to show that the method is viable if realistic initial data are provided.", "date": "2019-08-28", "date_type": "published", "id_number": "CaltechAUTHORS:20190828-133056303", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190828-133056303", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY 98-00737" }, { "agency": "NSF", "grant_number": "PHY 99-00672" }, { "agency": "NASA", "grant_number": "NAG5-7264" } ] }, "doi": "10.48550/arXiv.9912004", "primary_object": { "basename": "9912004.pdf", "url": "https://authors.library.caltech.edu/records/d6xq5-sx695/files/9912004.pdf" }, "resource_type": "monograph", "pub_year": "2019", "author_list": "Landry, Walter and Teukolsky, Saul A." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/tbbrs-nme46", "eprint_id": 98316, "eprint_status": "archive", "datestamp": "2023-08-19 19:44:07", "lastmod": "2023-10-18 17:15:04", "type": "monograph", "metadata_visibility": "show", "creators": { "items": [ { "id": "Duez-M-D", "name": { "family": "Duez", "given": "Matthew D." }, "orcid": "0000-0002-0050-1783" }, { "id": "Kidder-L-E", "name": { "family": "Kidder", "given": "Lawrence E." }, "orcid": "0000-0001-5392-7342" }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Evolving relativistic fluid spacetimes using pseudospectral methods and finite differencing", "ispublished": "unpub", "full_text_status": "public", "note": "This work was supported in part by a grant from the Sherman Fairchild Foundation, by NSF grants DMS-0553677, PHY-0354631, and NASA grant NNG05GG51G.\n\nSubmitted - 0702126.pdf
", "abstract": "We present a new code for solving the coupled Einstein-hydrodynamics equations to evolve relativistic, self-gravitating fluids. The Einstein field equations are solved on one grid using pseudospectral methods, while the fluids are evolved on another grid by finite differencing. We discuss implementation details, such as the communication between the grids and the treatment of stellar surfaces, and present code tests.", "date": "2019-08-28", "date_type": "published", "id_number": "CaltechAUTHORS:20190828-112436025", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190828-112436025", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Sherman Fairchild Foundation" }, { "agency": "NSF", "grant_number": "DMS-0553677" }, { "agency": "NSF", "grant_number": "PHY-0354631" }, { "agency": "NASA", "grant_number": "NNG05GG51G" } ] }, "doi": "10.48550/arXiv.0702126", "primary_object": { "basename": "0702126.pdf", "url": "https://authors.library.caltech.edu/records/tbbrs-nme46/files/0702126.pdf" }, "resource_type": "monograph", "pub_year": "2019", "author_list": "Duez, Matthew D.; Kidder, Lawrence E.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/4ewt3-zt209", "eprint_id": 89302, "eprint_status": "archive", "datestamp": "2023-08-19 16:18:20", "lastmod": "2023-10-18 22:39:32", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kumar-P", "name": { "family": "Kumar", "given": "Prayush" } }, { "id": "Blackman-J", "name": { "family": "Blackman", "given": "Jonathan" }, "orcid": "0000-0002-7113-0289" }, { "id": "Field-S-E", "name": { "family": "Field", "given": "Scott E." } }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark" } }, { "id": "Galley-C-R", "name": { "family": "Galley", "given": "Chad R." } }, { "id": "Boyle-M", "name": { "family": "Boyle", "given": "Michael" } }, { "id": "Kidder-L-E", "name": { "family": "Kidder", "given": "Lawrence E." }, "orcid": "0000-0001-5392-7342" }, { "id": "Pfeiffer-H-P", "name": { "family": "Pfeiffer", "given": "Harald P." }, "orcid": "0000-0001-9288-519X" }, { "id": "Szil\u00e1gyi-B", "name": { "family": "Szil\u00e1gyi", "given": "B\u00e9la" } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Constraining the parameters of GW150914 and GW170104 with numerical relativity surrogates", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2019 American Physical Society. \n\nReceived 25 September 2018; published 7 June 2019. \n\nWe gratefully acknowledge support for this research at Cornell from the Sherman Fairchild Foundation and NSF Grant No. PHY-1606654; at Caltech from the Sherman Fairchild Foundation and NSF Grant No. PHY-1404569; at CITA from NSERC of Canada, the Ontario Early Researcher Awards Program, the Canada Research Chairs Program, and the Canadian Institute for Advanced Research; and at Princeton from NSF Grant No. PHY-1305682 and the Simons Foundation. S. E. F. was partially supported by NSF Grant No. PHY-1806665. P. K. would like to thank FAPESP Grant No. 2016/01343-7 for hospitality during his visits to ICTP-SAIFR, where part of this work was completed. This research has made use of data, software and/or web tools obtained from the LIGO Open Science Center (https://losc.ligo.org), a service of LIGO Laboratory, the LIGO Scientific Collaboration, and the Virgo Collaboration. LIGO is funded by the U.S. National Science Foundation. Virgo is funded by the French Centre National de Recherche Scientifique (CNRS), the Italian Istituto Nazionale della Fisica Nucleare (INFN), and the Dutch Nikhef, with contributions by Polish and Hungarian institutes.\n\nPublished - PhysRevD.99.124005.pdf
Submitted - 1808.08004.pdf
Supplemental Material - GW170104_NRSur7dq2_RestrictedPriors.zip
", "abstract": "Gravitational-wave (GW) detectors have begun to observe coalescences of heavy black hole binaries (M \u2273 50\u2009\u2009M_\u2299) at a consistent pace for the past few years. Accurate models of gravitational waveforms are essential for unbiased and precise estimation of source parameters, such as masses and spins of component black holes. Recently developed surrogate models based on high-accuracy numerical relativity (NR) simulations provide ideal models for constraining physical parameters describing these heavy black hole merger events. In this paper, we first demonstrate the viability of these multi-modal surrogate models as reliable parameter estimation tools. We show that within a fully Bayesian framework, NR surrogates can help extract additional information from GW observations that is inaccessible to traditional models. We demonstrate this by analyzing a set of synthetic signals with NR surrogate templates and comparing against contemporary approximate models. We then consider the case of two of the earliest binary black holes detected by the LIGO observatories, GW150914 and GW170104. We reanalyze their data with the generically precessing NR-based surrogate model and freely provide the resulting posterior samples as supplemental material. We find that our refined analysis is able to extract information from sub-dominant GW harmonics in data, and therefore better resolve the degeneracy in measuring source luminosity distance and orbital inclination for both events. Our analysis estimates the sources of both events to be 20%\u201325% further away than was previously estimated. Our analysis also constrains their orbital orientations more tightly around face-on or face-off configurations than before. Additionally, for GW150914 we constrain the effective inspiral spin \u03c7_(eff) more tightly around zero. This work is one of the first to unambiguously extract sub-dominant GW mode information from real events. It is also a first step toward eliminating the approximations used in semi-analytic waveform models from GW parameter estimation. It strongly motivates that NR surrogates be extended to cover more of the binary black hole parameter space.", "date": "2019-06-15", "date_type": "published", "publication": "Physical Review D", "volume": "99", "number": "12", "publisher": "American Physical Society", "pagerange": "Art. No. 124005", "id_number": "CaltechAUTHORS:20180830-092941715", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180830-092941715", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Sherman Fairchild Foundation" }, { "agency": "NSF", "grant_number": "PHY-1606654" }, { "agency": "NSF", "grant_number": "PHY-1404569" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "Ontario Early Researcher Award" }, { "agency": "Canada Research Chairs Program" }, { "agency": "Canadian Institute for Advanced Research (CIFAR)" }, { "agency": "NSF", "grant_number": "PHY-1305682" }, { "agency": "Simons Foundation" }, { "agency": "NSF", "grant_number": "PHY-1806665" }, { "agency": "Funda\u00e7\u00e3o de Amparo \u00e0 Pesquisa do Estado de Sao Paulo (FAPESP)", "grant_number": "2016/01343-7" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Istituto Nazionale di Fisica Nucleare (INFN)" }, { "agency": "Nikhef" } ] }, "local_group": { "items": [ { "id": "Walter-Burke-Institute-for-Theoretical-Physics" }, { "id": "Astronomy-Department" } ] }, "doi": "10.1103/PhysRevD.99.124005", "primary_object": { "basename": "PhysRevD.99.124005.pdf", "url": "https://authors.library.caltech.edu/records/4ewt3-zt209/files/PhysRevD.99.124005.pdf" }, "related_objects": [ { "basename": "1808.08004.pdf", "url": "https://authors.library.caltech.edu/records/4ewt3-zt209/files/1808.08004.pdf" }, { "basename": "GW170104_NRSur7dq2_RestrictedPriors.zip", "url": "https://authors.library.caltech.edu/records/4ewt3-zt209/files/GW170104_NRSur7dq2_RestrictedPriors.zip" } ], "resource_type": "article", "pub_year": "2019", "author_list": "Kumar, Prayush; Blackman, Jonathan; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/6asv2-mgx35", "eprint_id": 92619, "eprint_status": "archive", "datestamp": "2023-08-19 14:45:49", "lastmod": "2023-10-20 15:54:52", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Okounkova-Maria", "name": { "family": "Okounkova", "given": "Maria" }, "orcid": "0000-0001-7869-5496" }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Numerical black hole initial data and shadows in dynamical Chern\u2013Simons gravity", "ispublished": "pub", "full_text_status": "public", "keywords": "general relativity, numerical relativity, black hole shadows, dynamical Chern\u2013Simons", "note": "\u00a9 2019 IOP Publishing Ltd. \n\nReceived 12 October 2018, revised 15 December 2018; Accepted for publication 9 January 2019; Published 4 February 2019. \n\nWe would like to thank Leo Stein for many useful discussions and providing us with the code used to generate the initial data in [32]. We would also like to thank Francois Hebert for helping us use the SXS lensing code. We thank Harald Pfeiffer and Leo Stein for careful reading of this manuscript. This work was supported in part by the Sherman Fairchild Foundation, and NSF grants PHY-1708212 and PHY-1708213 at Caltech and PHY-1606654 at Cornell. Computations were performed using the Spectral Einstein Code [30], including the Simulating Extreme Spacetimes collaboration lensing code [40]. All computations were performed on the Wheeler cluster at Caltech, which is supported by the Sherman Fairchild Foundation and by Caltech.\n\nAccepted Version - 1810.05306.pdf
", "abstract": "We present a scheme for generating first-order metric perturbation initial data for an arbitrary background and source. We then apply this scheme to derive metric perturbations in order-reduced dynamical Chern\u2013Simons gravity (dCS). In particular, we solve for metric perturbations on a black hole background that are sourced by a first-order dCS scalar field. This gives us the leading-order metric perturbation to the spacetime in dCS gravity. We then use these solutions to compute black hole shadows in the linearly perturbed spacetime by evolving null geodesics. We present a novel scheme to decompose the shape of the shadow into multipoles parametrized by the spin of the background black hole and the perturbation parameter . We find that we can differentiate the presence of a pure Kerr spacetime from a spacetime with a dCS perturbation using the shadow, allowing in part for a null-hypothesis test of general relativity. We then consider these results in the context of the event horizon telescope.", "date": "2019-03-07", "date_type": "published", "publication": "Classical and Quantum Gravity", "volume": "36", "number": "5", "publisher": "IOP", "pagerange": "Art. No. 054001", "id_number": "CaltechAUTHORS:20190204-094810196", "issn": "0264-9381", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190204-094810196", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY-1708212" }, { "agency": "NSF", "grant_number": "PHY-1708213" }, { "agency": "NSF", "grant_number": "PHY-1606654" }, { "agency": "Sherman Fairchild Foundation" }, { "agency": "Caltech" } ] }, "local_group": { "items": [ { "id": "Walter-Burke-Institute-for-Theoretical-Physics" }, { "id": "Astronomy-Department" } ] }, "doi": "10.1088/1361-6382/aafcdf", "primary_object": { "basename": "1810.05306.pdf", "url": "https://authors.library.caltech.edu/records/6asv2-mgx35/files/1810.05306.pdf" }, "resource_type": "article", "pub_year": "2019", "author_list": "Okounkova, Maria; Scheel, Mark A.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/3682y-rqx96", "eprint_id": 92955, "eprint_status": "archive", "datestamp": "2023-08-19 14:20:02", "lastmod": "2023-10-20 16:40:24", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Okounkova-Maria", "name": { "family": "Okounkova", "given": "Maria" }, "orcid": "0000-0001-7869-5496" }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Evolving metric perturbations in dynamical Chern-Simons gravity", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2019 American Physical Society. \n\nReceived 26 November 2018; published 14 February 2019. \n\nWe would like to thank Leo Stein for helpful discussions, providing us with the code used to generate the initial data in [26], and careful reading of this manuscript. We would also like to thank Luis Lehner for suggesting this project. This work was supported in part by the Sherman Fairchild Foundation and National Science Foundation Grants No. PHY-1708212 and No. PHY-1708213 at Caltech and No. PHY-1606654 at Cornell. Computations were performed using the Spectral Einstein Code [21]. All computations were performed on the Wheeler cluster at Caltech, which is supported by the Sherman Fairchild Foundation and by Caltech.\n\nPublished - PhysRevD.99.044019.pdf
Submitted - 1811.10713.pdf
", "abstract": "The stability of rotating black holes in dynamical Chern-Simons gravity (dCS) is an open question. To study this issue, we evolve the leading-order metric perturbation in order-reduced dynamical Chern-Simons gravity. The source is the leading-order dCS scalar field coupled to the spacetime curvature of a rotating black hole background. We use a well-posed, constraint-preserving scheme. We find that the leading-order metric perturbation numerically exhibits linear growth, but that the level of this growth converges to zero with numerical resolution. This analysis shows that spinning black holes in dCS gravity are numerically stable to leading-order perturbations in the metric.", "date": "2019-02-15", "date_type": "published", "publication": "Physical Review D", "volume": "99", "number": "4", "publisher": "American Physical Society", "pagerange": "Art. No. 044019", "id_number": "CaltechAUTHORS:20190215-112239838", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190215-112239838", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Sherman Fairchild Foundation" }, { "agency": "NSF", "grant_number": "PHY-1708212" }, { "agency": "NSF", "grant_number": "PHY-1708213" }, { "agency": "NSF", "grant_number": "PHY-1606654" } ] }, "local_group": { "items": [ { "id": "Walter-Burke-Institute-for-Theoretical-Physics" }, { "id": "Astronomy-Department" } ] }, "doi": "10.1103/PhysRevD.99.044019", "primary_object": { "basename": "1811.10713.pdf", "url": "https://authors.library.caltech.edu/records/3682y-rqx96/files/1811.10713.pdf" }, "related_objects": [ { "basename": "PhysRevD.99.044019.pdf", "url": "https://authors.library.caltech.edu/records/3682y-rqx96/files/PhysRevD.99.044019.pdf" } ], "resource_type": "article", "pub_year": "2019", "author_list": "Okounkova, Maria; Scheel, Mark A.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/5wr2p-vn933", "eprint_id": 89303, "eprint_status": "archive", "datestamp": "2023-08-19 13:54:43", "lastmod": "2023-10-18 22:39:35", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Deppe-N", "name": { "family": "Deppe", "given": "Nils" } }, { "id": "Kidder-L-E", "name": { "family": "Kidder", "given": "Lawrence E." }, "orcid": "0000-0001-5392-7342" }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Critical behavior in 3D gravitational collapse of massless scalar \n fields", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2019 American Physical Society.\n\nReceived 23 February 2018; published 10 January 2019.\n\nWe are grateful to Andy Bohn, Fran\u00e7ois H\u00e9bert, and Leo Stein for insightful discussions and feedback on earlier versions of this paper. We are also grateful to the anonymous referee for the feedback. This work was supported in part by a Natural Sciences and Engineering Research Council of Canada PGS-D grant to N.\u2009D., NSF Grant No. PHY-1606654 at Cornell University, and by a grant from the Sherman Fairchild Foundation. Computations were performed on the Zwicky cluster at Caltech, supported by the Sherman Fairchild Foundation and by NSF Grant No. PHY-0960291.\n\nPublished - PhysRevD.99.024018.pdf
Submitted - 1802.08682.pdf
", "abstract": "We present results from a study of critical behavior in 3D gravitational collapse with no symmetry assumptions. The source of the gravitational field is a massless scalar field. This is a well-studied case for spherically symmetric gravitational collapse, allowing us to understand the reliability and accuracy of the simulations. We study both supercritical and subcritical evolutions to see if one provides more accurate results than the other. We find that even for nonspherical initial data with 35% of the power in the \u2113=2 spherical harmonic, the critical solution is the same as in spherical symmetry.", "date": "2019-01-15", "date_type": "published", "publication": "Physical Review D", "volume": "99", "number": "2", "publisher": "American Physical Society", "pagerange": "Art. No. 024018", "id_number": "CaltechAUTHORS:20180830-093713741", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180830-093713741", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "NSF", "grant_number": "PHY-1606654" }, { "agency": "Sherman Fairchild Foundation" }, { "agency": "NSF", "grant_number": "PHY-0960291" } ] }, "local_group": { "items": [ { "id": "TAPIR" }, { "id": "Astronomy-Department" } ] }, "doi": "10.1103/PhysRevD.99.024018", "primary_object": { "basename": "1802.08682.pdf", "url": "https://authors.library.caltech.edu/records/5wr2p-vn933/files/1802.08682.pdf" }, "related_objects": [ { "basename": "PhysRevD.99.024018.pdf", "url": "https://authors.library.caltech.edu/records/5wr2p-vn933/files/PhysRevD.99.024018.pdf" } ], "resource_type": "article", "pub_year": "2019", "author_list": "Deppe, Nils; Kidder, Lawrence E.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/d2jvf-d4x27", "eprint_id": 86873, "eprint_status": "archive", "datestamp": "2023-08-19 11:04:52", "lastmod": "2023-10-18 20:39:44", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "H\u00e9bert-F", "name": { "family": "H\u00e9bert", "given": "Fran\u00e7ois" } }, { "id": "Kidder-L-E", "name": { "family": "Kidder", "given": "Lawrence E." }, "orcid": "0000-0001-5392-7342" }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "General-relativistic neutron star evolutions with the discontinuous Galerkin method", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2018 American Physical Society.\n\nReceived 5 April 2018; published 27 August 2018.\n\nWe thank Andy Bohn, Mike Boyle, Nils Deppe, Matt Duez, Francois Foucart, Jan Hesthaven, Curran Muhlberger, and Will Throwe for many helpful conversations through the course of this work. We gratefully acknowledge support for this research from the Sherman Fairchild Foundation; from NSF Grants No. PHY-1606654 and No. AST-1333129 at Cornell; and from NSF Grants No. PHY-1404569, No. PHY-1708212, and No. PHY-1708213 at Caltech. F.\u2009H. acknowledges support by the NSF Graduate Research Fellowship under Grant No. DGE-1144153. Computations were performed at Caltech on the Zwicky cluster, which is supported by the Sherman Fairchild Foundation and by NSF Grant No. PHY-0960291, and on the Wheeler cluster, which is supported by the Sherman Fairchild Foundation.\n\nPublished - PhysRevD.98.044041.pdf
Submitted - 1804.02003.pdf
", "abstract": "Simulations of relativistic hydrodynamics often need both high accuracy and robust shock-handling properties. The discontinuous Galerkin method combines these features\u2014a high order of convergence in regions where the solution is smooth and shock-capturing properties for regions where it is not\u2014with geometric flexibility and is therefore well suited to solve the partial differential equations describing astrophysical scenarios. We present here evolutions of a general-relativistic neutron star with the discontinuous Galerkin method. In these simulations, we simultaneously evolve the spacetime geometry and the matter on the same computational grid, which we conform to the spherical geometry of the problem. To verify the correctness of our implementation, we perform standard convergence and shock tests. We then show results for evolving, in three dimensions, a Kerr black hole; a neutron star in the Cowling approximation (holding the spacetime metric fixed); and, finally, a neutron star where the spacetime and matter are both dynamical. The evolutions show long-term stability, good accuracy, and an improved rate of convergence versus a comparable-resolution finite-volume method.", "date": "2018-08-15", "date_type": "published", "publication": "Physical Review D", "volume": "98", "number": "4", "publisher": "American Physical Society", "pagerange": "Art. No. 044041", "id_number": "CaltechAUTHORS:20180606-164721712", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180606-164721712", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Sherman Fairchild Foundation" }, { "agency": "NSF", "grant_number": "PHY-1606654" }, { "agency": "NSF", "grant_number": "AST-1333129" }, { "agency": "NSF", "grant_number": "PHY-1404569" }, { "agency": "NSF", "grant_number": "PHY-1708212" }, { "agency": "NSF", "grant_number": "PHY-1708213" }, { "agency": "NSF Graduate Research Fellowship", "grant_number": "DGE-1144153" }, { "agency": "NSF", "grant_number": "PHY-0960291" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.1103/PhysRevD.98.044041", "primary_object": { "basename": "1804.02003.pdf", "url": "https://authors.library.caltech.edu/records/d2jvf-d4x27/files/1804.02003.pdf" }, "related_objects": [ { "basename": "PhysRevD.98.044041.pdf", "url": "https://authors.library.caltech.edu/records/d2jvf-d4x27/files/PhysRevD.98.044041.pdf" } ], "resource_type": "article", "pub_year": "2018", "author_list": "H\u00e9bert, Fran\u00e7ois; Kidder, Lawrence E.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/aqr51-j7v22", "eprint_id": 86703, "eprint_status": "archive", "datestamp": "2023-08-19 09:15:16", "lastmod": "2023-10-18 19:54:45", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bhagwat-S", "name": { "family": "Bhagwat", "given": "Swetha" } }, { "id": "Okounkova-M", "name": { "family": "Okounkova", "given": "Maria" } }, { "id": "Ballmer-S-W", "name": { "family": "Ballmer", "given": "Stefan W." } }, { "id": "Brown-D-A", "name": { "family": "Brown", "given": "Duncan A." }, "orcid": "0000-0002-9180-5765" }, { "id": "Giesler-M-D", "name": { "family": "Giesler", "given": "Matthew" }, "orcid": "0000-0003-2300-893X" }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "On choosing the start time of binary black hole ringdowns", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2018 American Physical Society. \n\nReceived 7 November 2017; published 30 May 2018. \n\nWe would like to thank Alfonso Garc\u00eda-Parrado G\u00f3mez-Lobo, Kevin Barkett, Mike Boyle, Yanbei Chen, Joshua Goldberg, Casey Handmer, Daniel Hemberger, Maximilliano Isi, Badri Krishnan, Nicholas Meyer, Harald Pfeiffer, Leo Stein and Vijay Varma for many valuable conversations. In particular, we would like to thank Mike Boyle, Casey Handmer, Harald Pfeiffer, and Leo Stein for careful reading of this manuscript. We would like to thank William East for helping to generate the QNM metrics, and Geoffrey Lovelace for supplying the BBH simulation data used in this study. This work was supported in part by the Sherman Fairchild Foundation, the Brinson Foundation, NSF Grants No. PHY-1404569 and No. AST-1333520 at Caltech, and NSF Grant No. PHY-1606654 at Cornell University and Grants No. PHY-1404395, No. PHY-1707954 and No. PHY-1352511 at Syracuse University. M.\u2009O. gratefully acknowledges the support of the Dominic Orr Graduate Fellowship at Caltech. We used SpEC (Spectral Einstein Code) to perform the simulations and analysis [81]. Computations were performed on the Zwicky and Wheeler clusters at Caltech, which are supported by the Sherman Fairchild Foundation and by NSF Grant No. PHY-0960291. The BBH simulation was performed on the ORCA cluster at California State University, Fullerton (CSUF), supported by CSUF, NSF Grant No. PHY-142987, and the Research Corporation for Science Advancement.\n\nPublished - PhysRevD.97.104065.pdf
Submitted - 1711.00926.pdf
", "abstract": "The final stage of a binary black hole merger is ringdown, in which the system is described by a Kerr black hole with quasinormal mode perturbations. It is far from straightforward to identify the time at which the ringdown begins. Yet determining this time is important for precision tests of the general theory of relativity that compare an observed signal with quasinormal mode descriptions of the ringdown, such as tests of the no-hair theorem. We present an algorithmic method to analyze the choice of ringdown start time in the observed waveform. This method is based on determining how close the strong field is to a Kerr black hole (Kerrness). Using numerical relativity simulations, we characterize the Kerrness of the strong-field region close to the black hole using a set of local, gauge-invariant geometric and algebraic conditions that measure local isometry to Kerr. We produce a map that associates each time in the gravitational waveform with a value of each of these Kerrness measures; this map is produced by following outgoing null characteristics from the strong and near-field regions to the wave zone. We perform this analysis on a numerical relativity simulation with parameters consistent with GW150914\u2014the first gravitational-wave detection. We find that the choice of ringdown start time of 3 ms after merger used in the GW150914 study [B.\u2009P. Abbott et al. (Virgo Collaboration and LIGO Scientific Collaboration), Phys. Rev. Lett. 116, 221101 (2016).] to test general relativity corresponds to a high dimensionless perturbation amplitude of \u223c7.5\u00d710^(-3) in the strong-field region. This suggests that in higher signal-to-noise detections, one would need to start analyzing the signal at a later time for studies that depend on the validity of black hole perturbation theory.", "date": "2018-05-15", "date_type": "published", "publication": "Physical Review D", "volume": "97", "number": "10", "publisher": "American Physical Society", "pagerange": "Art. No. 104065", "id_number": "CaltechAUTHORS:20180530-091329126", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180530-091329126", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Sherman Fairchild Foundation" }, { "agency": "Brinson Foundation" }, { "agency": "NSF", "grant_number": "PHY-1404569" }, { "agency": "NSF", "grant_number": "AST-1333520" }, { "agency": "NSF", "grant_number": "PHY-1606654" }, { "agency": "NSF", "grant_number": "PHY-1404395" }, { "agency": "NSF", "grant_number": "PHY-1707954" }, { "agency": "NSF", "grant_number": "PHY-1352511" }, { "agency": "Dominic Orr Graduate Fellowship" }, { "agency": "NSF", "grant_number": "PHY-0960291" }, { "agency": "California State University, Fullerton" }, { "agency": "NSF", "grant_number": "PHY-142987" }, { "agency": "Research Corporation" } ] }, "local_group": { "items": [ { "id": "Walter-Burke-Institute-for-Theoretical-Physics" }, { "id": "Astronomy-Department" } ] }, "doi": "10.1103/PhysRevD.97.104065", "primary_object": { "basename": "1711.00926.pdf", "url": "https://authors.library.caltech.edu/records/aqr51-j7v22/files/1711.00926.pdf" }, "related_objects": [ { "basename": "PhysRevD.97.104065.pdf", "url": "https://authors.library.caltech.edu/records/aqr51-j7v22/files/PhysRevD.97.104065.pdf" } ], "resource_type": "article", "pub_year": "2018", "author_list": "Bhagwat, Swetha; Okounkova, Maria; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/ejm07-qa216", "eprint_id": 85450, "eprint_status": "archive", "datestamp": "2023-08-19 08:21:28", "lastmod": "2023-10-18 18:14:30", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Healy-J-H", "name": { "family": "Healy", "given": "J." } }, { "id": "Lange-J", "name": { "family": "Lange", "given": "J." } }, { "id": "O'Shaughnessy-Richard", "name": { "family": "O'Shaughnessy", "given": "R." }, "orcid": "0000-0001-5832-8517" }, { "id": "Lousto-C-O", "name": { "family": "Lousto", "given": "C. O." } }, { "id": "Campanelli-M", "name": { "family": "Campanelli", "given": "M." } }, { "id": "Williamson-A-R", "name": { "family": "Williamson", "given": "A. R." } }, { "id": "Zlochower-Y", "name": { "family": "Zlochower", "given": "Y." } }, { "id": "Calder\u00f3n-Bustillo-J", "name": { "family": "Calder\u00f3n Bustillo", "given": "J." } }, { "id": "Clark-James-A", "name": { "family": "Clark", "given": "J. A." }, "orcid": "0000-0003-3243-1393" }, { "id": "Evans-Ciaran", "name": { "family": "Evans", "given": "C." }, "orcid": "0000-0003-3256-011X" }, { "id": "Ferguson-D", "name": { "family": "Ferguson", "given": "D." } }, { "id": "Ghonge-S", "name": { "family": "Ghonge", "given": "S." } }, { "id": "Jani-K", "name": { "family": "Jani", "given": "K." } }, { "id": "Khamesra-B", "name": { "family": "Khamesra", "given": "B." } }, { "id": "Laguna-P", "name": { "family": "Laguna", "given": "P." } }, { "id": "Shoemaker-D-M", "name": { "family": "Shoemaker", "given": "D. M." } }, { "id": "Boyle-M", "name": { "family": "Boyle", "given": "M." } }, { "id": "Garc\u00eda-A", "name": { "family": "Garc\u00eda", "given": "A." } }, { "id": "Hemberger-D-A", "name": { "family": "Hemberger", "given": "D. A." } }, { "id": "Kidder-Lawrence-E", "name": { "family": "Kidder", "given": "L. E." }, "orcid": "0000-0001-5392-7342" }, { "id": "Kumar-P", "name": { "family": "Kumar", "given": "P." } }, { "id": "Lovelace-Geoffrey", "name": { "family": "Lovelace", "given": "G." }, "orcid": "0000-0002-7084-1070" }, { "id": "Pfeiffer-Harald-P", "name": { "family": "Pfeiffer", "given": "H. P." }, "orcid": "0000-0001-9288-519X" }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "M. A." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "S. A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Targeted numerical simulations of binary black holes for GW170104", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2018 American Physical Society. \n\nReceived 15 December 2017; published 23 March 2018. \n\nThe authors thank S. Husa, C. Berry, K. Chatziioannou, and A. Zimmerman for their feedback on this work. The RIT authors gratefully acknowledge the NSF for financial support from Grants No. PHY-1607520, No. PHY-1707946, No. ACI-1550436, No. AST-1516150, No. ACI-1516125, and No. PHY-1726215. This work used the Extreme Science and Engineering Discovery Environment (XSEDE) [allocation TG-PHY060027N], which is supported by NSF Grant No. ACI-1548562. Computational resources were also provided by the NewHorizons and BlueSky Clusters at the Rochester Institute of Technology, which were supported by NSF Grants No. PHY-0722703, No. DMS-0820923, No. AST-1028087, and No. PHY-1229173. R.\u2009O.\u2009S. is supported by NSF Grants No. AST-1412449, No. PHY-1505629, and No. PHY-1607520. The GT authors gratefully acknowledge NSF support through Grants No. PHY-1505824, No. 1505524, and No. XSEDE TG-PHY120016. They also gratefully acknowledge support from the Cullen-Peck and Dunn Families. The SXS Collaboration authors gratefully acknowledge the Sherman Fairchild Foundation and NSF for financial support from Grants No. PHY-1307489, No. PHY-1606522, No. PHY-1606654, and No. AST-1333129. They also gratefully acknowledge support for this research at CITA from NSERC of Canada, the Ontario Early Researcher Awards Program, the Canada Research Chairs Program, and the Canadian Institute for Advanced Research. Calculations were done on the ORCA computer cluster, supported by NSF Grant No. PHY-1429873, the Research Corporation for Science Advancement, CSU Fullerton, the GPC supercomputer at the SciNet HPC Consortium [113]; SciNet is funded by the Canada Foundation for Innovation (CFI) under the auspices of Compute Canada; the Government of Ontario; Ontario Research Fund (ORF)\u2014Research Excellence; and the University of Toronto. Further calculations were performed on the Briar\u00e9e cluster at Sherbrooke University, managed by Calcul Qu\u00e9bec and Compute Canada and with operation funded by the Canada Foundation for Innovation (CFI), Minist\u00e9re de l'\u00c9conomie, de l'Innovation et des Exportations du Quebec (MEIE), RMGA and the Fonds de recherche du Qu\u00e9bec\u2014Nature et Technologies (FRQ-NT).\n\nPublished - PhysRevD.97.064027.pdf
Submitted - 1712.05836.pdf
", "abstract": "In response to LIGO's observation of GW170104, we performed a series of full numerical simulations of binary black holes, each designed to replicate likely realizations of its dynamics and radiation. These simulations have been performed at multiple resolutions and with two independent techniques to solve Einstein's equations. For the nonprecessing and precessing simulations, we demonstrate the two techniques agree mode by mode, at a precision substantially in excess of statistical uncertainties in current LIGO's observations. Conversely, we demonstrate our full numerical solutions contain information which is not accurately captured with the approximate phenomenological models commonly used to infer compact binary parameters. To quantify the impact of these differences on parameter inference for GW170104 specifically, we compare the predictions of our simulations and these approximate models to LIGO's observations of GW170104.", "date": "2018-03-15", "date_type": "published", "publication": "Physical Review D", "volume": "97", "number": "6", "publisher": "American Physical Society", "pagerange": "Art. No. 064027", "id_number": "CaltechAUTHORS:20180327-091526389", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180327-091526389", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY-1607520" }, { "agency": "NSF", "grant_number": "PHY-1707946" }, { "agency": "NSF", "grant_number": "ACI-1550436" }, { "agency": "NSF", "grant_number": "AST-1516150" }, { "agency": "NSF", "grant_number": "ACI-1516125" }, { "agency": "NSF", "grant_number": "PHY-1726215" }, { "agency": "NSF", "grant_number": "TG-PHY060027N" }, { "agency": "NSF", "grant_number": "ACI-1548562" }, { "agency": "NSF", "grant_number": "PHY-0722703" }, { "agency": "NSF", "grant_number": "DMS-0820923" }, { "agency": "NSF", "grant_number": "AST-1028087" }, { "agency": "NSF", "grant_number": "PHY-1229173" }, { "agency": "NSF", "grant_number": "AST-1412449" }, { "agency": "NSF", "grant_number": "PHY-1505629" }, { "agency": "NSF", "grant_number": "PHY-1607520" }, { "agency": "NSF", "grant_number": "PHY-1505824" }, { "agency": "NSF", "grant_number": "PHY-1505524" }, { "agency": "NSF", "grant_number": "TG-PHY120016" }, { "agency": "Cullen-Peck Family" }, { "agency": "Dunn Family" }, { "agency": "Sherman Fairchild Foundation" }, { "agency": "NSF", "grant_number": "PHY-1307489" }, { "agency": "NSF", "grant_number": "PHY-1606522" }, { "agency": "NSF", "grant_number": "PHY-1606654" }, { "agency": "NSF", "grant_number": "AST-1333129" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "Ontario Early Researcher Awards Program" }, { "agency": "Canada Research Chairs Program" }, { "agency": "Canadian Institute for Advanced Research (CIFAR)" }, { "agency": "NSF", "grant_number": "PHY-1429873" }, { "agency": "Research Corporation" }, { "agency": "California State University, Fullerton" }, { "agency": "SciNet HPC Consortium" }, { "agency": "Canada Foundation for Innovation" }, { "agency": "Compute Canada" }, { "agency": "Government of Ontario" }, { "agency": "Ontario Research Fund" }, { "agency": "University of Toronto" }, { "agency": "Minist\u00e9re de l'\u00c9conomie, de l'Innovation et des Exportations du Quebec (MEIE)" }, { "agency": "RMGA" }, { "agency": "Fonds de recherche du Qu\u00e9bec-Nature et Technologies (FRQ-NT)" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.1103/PhysRevD.97.064027", "primary_object": { "basename": "1712.05836.pdf", "url": "https://authors.library.caltech.edu/records/ejm07-qa216/files/1712.05836.pdf" }, "related_objects": [ { "basename": "PhysRevD.97.064027.pdf", "url": "https://authors.library.caltech.edu/records/ejm07-qa216/files/PhysRevD.97.064027.pdf" } ], "resource_type": "article", "pub_year": "2018", "author_list": "Healy, J.; Lange, J.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/bqeyv-95v77", "eprint_id": 83431, "eprint_status": "archive", "datestamp": "2023-08-19 06:04:02", "lastmod": "2023-10-17 23:07:21", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Lange-J", "name": { "family": "Lange", "given": "J." } }, { "id": "Hemberger-D-A", "name": { "family": "Hemberger", "given": "D. A." } }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "M. A." } }, { "id": "Szil\u00e1gyi-B", "name": { "family": "Szil\u00e1gyi", "given": "B." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "S." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Parameter estimation method that directly compares gravitational wave observations to numerical relativity", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2017 American Physical Society. \n\nReceived 26 May 2017; published 22 November 2017. \n\nThe RIT authors gratefully acknowledge the NSF for financial support from Grants No. PHY-1505629, No. AST-1664362, No. PHY-1607520, No. ACI-1550436, No. AST-1516150, and No. ACI-1516125. Computational resources were provided by XSEDE allocation Grant No. TG-PHY060027N, and by NewHorizons and BlueSky Clusters at Rochester Institute of Technology, which were supported by NSF Grants No. PHY-0722703, No. DMS-0820923, No. AST-1028087, and No. PHY-1229173. This research was also part of the Blue Waters sustained-petascale computing NSF projects Grants No. ACI-0832606, No. ACI-1238993, No. OCI-1515969, and No. OCI-0725070. \n\nThe SXS Collaboration authors gratefully acknowledge the NSF for financial support from Grants No. PHY-1307489, No. PHY-1606522, No. PHY-1606654, and No. AST- 1333129. They also gratefully acknowledge support for this research at CITA from NSERC of Canada, the Ontario Early Researcher Awards Program, the Canada Research Chairs Program, and the Canadian Institute for Advanced Research. Calculations were done on the ORCA computer cluster, supported by NSF Grant No. PHY-1429873, the Research Corporation for Science Advancement, CSU Fullerton, the GPC supercomputer at the SciNet HPC Consortium [49]; SciNet is funded by the Canada Foundation for Innovation (CFI) under the auspices of Compute Canada, the Government of Ontario, Ontario Research Fund (ORF)\u2014Research Excellence, and the University of Toronto. Further calculations were performed on the Briar\u00e9e cluster at Sherbrooke University, managed by Calcul Qu\u00e9bec and Compute Canada and with operation funded by the CFI, Minist\u00e9re de l'\u00c9conomie, de l'Innovation et des Exportations du Quebec (MEIE), RMGA and the Fonds de recherche du Qu\u00e9bec\u2014Nature et Technologies (FRQ-NT). \n\nThe GT authors gratefully acknowledge the NSF for financial support from Grants No. ACI-1550461 and No. PHY-1505824. Computational resources were provided by XSEDE and the Georgia Tech Cygnus Cluster. \n\nFinally, the authors are grateful for computational resources used for the parameter estimation runs provided by the Leonard E. Parker Center for Gravitation, Cosmology and Astrophysics at the University of Wisconsin\u2014Milwaukee, the Albert Einstein Institute at Hanover, Germany, and the California Institute of Technology at Pasadena, California.\n\nPublished - PhysRevD.96.104041.pdf
Submitted - 1705.09833.pdf
", "abstract": "We present and assess a Bayesian method to interpret gravitational wave signals from binary black holes. Our method directly compares gravitational wave data to numerical relativity (NR) simulations. In this study, we present a detailed investigation of the systematic and statistical parameter estimation errors of this method. This procedure bypasses approximations used in semianalytical models for compact binary coalescence. In this work, we use the full posterior parameter distribution for only generic nonprecessing binaries, drawing inferences away from the set of NR simulations used, via interpolation of a single scalar quantity (the marginalized log likelihood, lnL) evaluated by comparing data to nonprecessing binary black hole simulations. We also compare the data to generic simulations, and discuss the effectiveness of this procedure for generic sources. We specifically assess the impact of higher order modes, repeating our interpretation with both l \u2264 2 as well as l \u2264 3 harmonic modes. Using the l \u2264 3 higher modes, we gain more information from the signal and can better constrain the parameters of the gravitational wave signal. We assess and quantify several sources of systematic error that our procedure could introduce, including simulation resolution and duration; most are negligible. We show through examples that our method can recover the parameters for equal mass, zero spin, GW150914-like, and unequal mass, precessing spin sources. Our study of this new parameter estimation method demonstrates that we can quantify and understand the systematic and statistical error. This method allows us to use higher order modes from numerical relativity simulations to better constrain the black hole binary parameters.", "date": "2017-11-15", "date_type": "published", "publication": "Physical Review D", "volume": "96", "number": "10", "publisher": "American Physical Society", "pagerange": "Art. No. 104041", "id_number": "CaltechAUTHORS:20171122-095738196", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20171122-095738196", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY-1505629" }, { "agency": "NSF", "grant_number": "AST-1664362" }, { "agency": "NSF", "grant_number": "PHY-1607520" }, { "agency": "NSF", "grant_number": "ACI-1550436" }, { "agency": "NSF", "grant_number": "AST-1516150" }, { "agency": "NSF", "grant_number": "ACI-1516125" }, { "agency": "NSF", "grant_number": "TG-PHY060027N" }, { "agency": "NSF", "grant_number": "PHY-0722703" }, { "agency": "NSF", "grant_number": "DMS-0820923" }, { "agency": "NSF", "grant_number": "AST-1028087" }, { "agency": "NSF", "grant_number": "PHY-1229173" }, { "agency": "NSF", "grant_number": "ACI-0832606" }, { "agency": "NSF", "grant_number": "ACI-1238993" }, { "agency": "NSF", "grant_number": "OCI-1515969" }, { "agency": "NSF", "grant_number": "OCI-0725070" }, { "agency": "NSF", "grant_number": "PHY-1307489" }, { "agency": "NSF", "grant_number": "PHY-1606522" }, { "agency": "NSF", "grant_number": "PHY-1606654" }, { "agency": "NSF", "grant_number": "AST-1333129" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "Ontario Early Researcher Awards Program" }, { "agency": "Canada Research Chairs Program" }, { "agency": "Canadian Institute for Advanced Research (CIFAR)" }, { "agency": "NSF", "grant_number": "PHY-1429873" }, { "agency": "Research Corporation" }, { "agency": "California State University, Fullerton" }, { "agency": "Canada Foundation for Innovation" }, { "agency": "Compute Canada" }, { "agency": "Government of Ontario" }, { "agency": "Ontario Research Fund" }, { "agency": "University of Toronto" }, { "agency": "Minist\u00e9re de l'\u00c9conomie, de l'Innovation et des Exportations du Quebec (MEIE)" }, { "agency": "RMGA" }, { "agency": "Fonds de recherche du Qu\u00e9bec-Nature et Technologies (FRQ-NT)" }, { "agency": "NSF", "grant_number": "ACI-1550461" }, { "agency": "NSF", "grant_number": "PHY-1505824" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.1103/PhysRevD.96.104041", "primary_object": { "basename": "PhysRevD.96.104041.pdf", "url": "https://authors.library.caltech.edu/records/bqeyv-95v77/files/PhysRevD.96.104041.pdf" }, "related_objects": [ { "basename": "1705.09833.pdf", "url": "https://authors.library.caltech.edu/records/bqeyv-95v77/files/1705.09833.pdf" } ], "resource_type": "article", "pub_year": "2017", "author_list": "Lange, J.; Hemberger, D. A.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/zbkyq-2ye27", "eprint_id": 76537, "eprint_status": "archive", "datestamp": "2023-08-19 03:10:20", "lastmod": "2023-10-25 16:05:39", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Abbott-B-P", "name": { "family": "Abbott", "given": "B. P." } }, { "id": "Abbott-R", "name": { "family": "Abbott", "given": "R." } }, { "id": "Adhikari-R-X", "name": { "family": "Adhikari", "given": "R. X." }, "orcid": "0000-0002-5731-5076" }, { "id": "Ananyeva-A", "name": { "family": "Ananyeva", "given": "A." } }, { "id": "Anderson-S-B", "name": { "family": "Anderson", "given": "S. B." } }, { "id": "Appert-S", "name": { "family": "Appert", "given": "S." } }, { "id": "Arai-Koji", "name": { "family": "Arai", "given": "K." }, "orcid": "0000-0001-8916-8915" }, { "id": "Araya-M-C", "name": { "family": "Araya", "given": "M. C." } }, { "id": "Barayoga-J-C", "name": { "family": "Barayoga", "given": "J. C." } }, { "id": "Barish-B-C", "name": { "family": "Barish", "given": "B. C." } }, { "id": "Berger-B-K", "name": { "family": "Berger", "given": "B. K." } }, { "id": "Billingsley-G", "name": { "family": "Billingsley", "given": "G." }, "orcid": "0000-0002-4141-2744" }, { "id": "Biscans-S", "name": { "family": "Biscans", "given": "S" }, "orcid": "0000-0002-9635-7527" }, { "id": "Blackburn-J-K", "name": { "family": "Blackburn", "given": "J. K." }, "orcid": "0000-0002-3838-2986" }, { "id": "Bork-R", "name": { "family": "Bork", "given": "R." } }, { "id": "Brooks-A-F", "name": { "family": "Brooks", "given": "A. F." }, "orcid": "0000-0003-4295-792X" }, { "id": "Brunett-S", "name": { "family": "Brunett", "given": "S." } }, { "id": "Cahillane-C", "name": { "family": "Cahillane", "given": "C." } }, { "id": "Callister-T-A", "name": { "family": "Callister", "given": "T. A." }, "orcid": "0000-0001-9892-177X" }, { "id": "Cepeda-C-B", "name": { "family": "Cepeda", "given": "C. B." } }, { "id": "Couvares-P", "name": { "family": "Couvares", "given": "P." } }, { "id": "Coyne-D-C", "name": { "family": "Coyne", "given": "D. C." }, "orcid": "0000-0002-6427-3222" }, { "id": "Drever-R-W-P", "name": { "family": "Drever", "given": "R. W. P." } }, { "id": "Ehrens-P", "name": { "family": "Ehrens", "given": "P." } }, { "id": "Eichholz-J", "name": { "family": "Eichholz", "given": "J." } }, { "id": "Etzel-T", "name": { "family": "Etzel", "given": "T." } }, { "id": "Fries-E-M", "name": { "family": "Fries", "given": "E. M." } }, { "id": "Gossan-S-E", "name": { "family": "Gossan", "given": "S. E." }, "orcid": "0000-0002-8138-9198" }, { "id": "Gushwa-K-E", "name": { "family": "Gushwa", "given": "K. E." } }, { "id": "Gustafson-E-K", "name": { "family": "Gustafson", "given": "E. K." } }, { "id": "Hall-E-D", "name": { "family": "Hall", "given": "E. D." }, "orcid": "0000-0001-9018-666X" }, { "id": "Heptonstall-A-W", "name": { "family": "Heptonstall", "given": "A. W." } }, { "id": "Isi-M", "name": { "family": "Isi", "given": "M." }, "orcid": "0000-0001-8830-8672" }, { "id": "Kanner-J-B", "name": { "family": "Kanner", "given": "J. B." }, "orcid": "0000-0001-8115-0577" }, { "id": "Kondrashov-V", "name": { "family": "Kondrashov", "given": "V." } }, { "id": "Korth-W-Z", "name": { "family": "Korth", "given": "W. Z." }, "orcid": "0000-0003-3527-1348" }, { "id": "Kozak-D-B", "name": { "family": "Kozak", "given": "D. B." }, "orcid": "0000-0003-3118-8950" }, { "id": "Lazzarini-A", "name": { "family": "Lazzarini", "given": "A." } }, { "id": "Maros-E", "name": { "family": "Maros", "given": "E." } }, { "id": "Massinger-T-J", "name": { "family": "Massinger", "given": "T. J." }, "orcid": "0000-0002-3429-5025" }, { "id": "Matichard-F", "name": { "family": "Matichard", "given": "F." } }, { "id": "McIntyre-G", "name": { "family": "McIntyre", "given": "G." } }, { "id": "McIver-J", "name": { "family": "McIver", "given": "J." }, "orcid": "0000-0003-0316-1355" }, { "id": "Meshkov-S", "name": { "family": "Meshkov", "given": "S." } }, { "id": "Pedraza-M", "name": { "family": "Pedraza", "given": "M." } }, { "id": "Perreca-A", "name": { "family": "Perreca", "given": "A." } }, { "id": "Quintero-E-A", "name": { "family": "Quintero", "given": "E. A." } }, { "id": "Reitze-D-H", "name": { "family": "Reitze", "given": "D. H." } }, { "id": "Robertson-N-A", "name": { "family": "Robertson", "given": "N. A." } }, { "id": "Rollins-J-G", "name": { "family": "Rollins", "given": "J. G." } }, { "id": "Sachdev-S", "name": { "family": "Sachdev", "given": "S." }, "orcid": "0000-0002-2432-7070" }, { "id": "Sanchez-E-J", "name": { "family": "Sanchez", "given": "E. J." } }, { "id": "Schmidt-P", "name": { "family": "Schmidt", "given": "P." } }, { "id": "Singer-A", "name": { "family": "Singer", "given": "A." } }, { "id": "Smith-R-J-E", "name": { "family": "Smith", "given": "R. J. E." } }, { "id": "Taylor-R", "name": { "family": "Taylor", "given": "R." } }, { "id": "Torrie-C-I", "name": { "family": "Torrie", "given": "C. I." } }, { "id": "Tso-Rhondale", "name": { "family": "Tso", "given": "R." }, "orcid": "0000-0003-4464-0117" }, { "id": "Urban-A-L", "name": { "family": "Urban", "given": "A. L." } }, { "id": "Vajente-G", "name": { "family": "Vajente", "given": "G." }, "orcid": "0000-0002-7656-6882" }, { "id": "Vass-S", "name": { "family": "Vass", "given": "S." } }, { "id": "Venugopalan-G", "name": { "family": "Venugopalan", "given": "G." } }, { "id": "Wade-A-R", "name": { "family": "Wade", "given": "A. R." } }, { "id": "Wallace-L", "name": { "family": "Wallace", "given": "L." } }, { "id": "Weinstein-Alan-J-Physics", "name": { "family": "Weinstein", "given": "A. J." }, "orcid": "0000-0002-0928-6784" }, { "id": "Williams-R-D", "name": { "family": "Williams", "given": "R. D." }, "orcid": "0000-0002-9145-8580" }, { "id": "Wipf-C-C", "name": { "family": "Wipf", "given": "C. C." } }, { "id": "Yamamoto-Hiroaki", "name": { "family": "Yamamoto", "given": "H." } }, { "id": "Zhang-Liyuan", "name": { "family": "Zhang", "given": "L." }, "orcid": "0000-0002-0898-787X" }, { "id": "Zucker-M-E", "name": { "family": "Zucker", "given": "M. E." }, "orcid": "0000-0002-2544-1596" }, { "id": "Zweizig-J", "name": { "family": "Zweizig", "given": "J." }, "orcid": "0000-0002-1521-3397" }, { "id": "Blackman-J", "name": { "family": "Blackman", "given": "J." }, "orcid": "0000-0002-7113-0289" }, { "id": "Chen-Yanbei", "name": { "family": "Chen", "given": "Y." }, "orcid": "0000-0002-9730-9463" }, { "id": "Ma-Yiqiu", "name": { "family": "Ma", "given": "Y." }, "orcid": "0000-0001-7192-4874" }, { "id": "Varma-V", "name": { "family": "Varma", "given": "V." }, "orcid": "0000-0002-9994-1761" }, { "id": "Hemberger-D-A", "name": { "family": "Hemberger", "given": "D." } }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "M." } }, { "id": "Szilagyi-B", "name": { "family": "Szilagyi", "given": "B." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "S." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Effects of waveform model systematics on the interpretation of GW150914", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2017 IOP Publishing Ltd. \n\nReceived 16 December 2016. Accepted 22 March 2017. Accepted Manuscript online 22 March 2017. Published 12 April 2017. \n\nFocus issue: Gravitational waves. \nGuest editors: P Shawhan, D Shoemaker \n\nThe authors gratefully acknowledge the support of the United States National Science Foundation (NSF) for the construction and operation of the LIGO Laboratory and Advanced LIGO as well as the Science and Technology Facilities Council (STFC) of the United Kingdom, the Max-Planck-Society (MPS), and the State of Niedersachsen/Germany for support of the construction of Advanced LIGO and construction and operation of the GEO600 detector. Additional support for Advanced LIGO was provided by the Australian Research Council. The authors gratefully acknowledge the Italian Istituto Nazionale di Fisica Nucleare (INFN), the French Centre National de la Recherche Scientifique (CNRS) and the Foundation for Fundamental Research on Matter supported by the Netherlands Organisation for Scientific Research, for the construction and operation of the Virgo detector and the creation and support of the EGO consortium. The authors also gratefully acknowledge research support from these agencies as well as by the Council of Scientific and Industrial Research of India, Department of Science and Technology, India, Science & Engineering Research Board (SERB), India, Ministry of Human Resource Development, India, the Spanish Ministerio de Econom\u00eda y Competitividad, the Conselleria d'Economia i Competitivitat and Conselleria d'Educaci\u00f3, Cultura i Universitats of the Govern de les Illes Balears, the National Science Centre of Poland, the European Commission, the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, the Hungarian Scientific Research Fund (OTKA), the Lyon Institute of Origins (LIO), the National Research Foundation of Korea, Industry Canada and the Province of Ontario through the Ministry of Economic Development and Innovation, the Natural Science and Engineering Research Council Canada, Canadian Institute for Advanced Research, the Brazilian Ministry of Science, Technology, and Innovation, Funda\u00e7\u00e3o de Amparo \u00e0 Pesquisa do Estado de S\u00e3o Paulo (FAPESP), Russian Foundation for Basic Research, the Leverhulme Trust, the Research Corporation, Ministry of Science and Technology (MOST), Taiwan and the Kavli Foundation. The authors gratefully acknowledge the support of the NSF, STFC, MPS, INFN, CNRS and the State of Niedersachsen/Germany for provision of computational resources. \n\nCFUIB simulations were carried out on the UK DiRAC Datacentric cluster. The SXS simulations were carried out on HPC resources provided by Compute Canada, the Research Corporation, and California State University Fullerton, on the San Diego Supercomputer Center's machine Comet and on the AEI Datura cluster. We further acknowledge support from the Research Corporation for Science Advancement, and the Sherman Fairchild Foundation.\n\nSubmitted - 1611.07531.pdf
", "abstract": "Parameter estimates of GW150914 were obtained using Bayesian inference, based on three semi-analytic waveform models for binary black hole coalescences. These waveform models differ from each other in their treatment of black hole spins, and all three models make some simplifying assumptions, notably to neglect sub-dominant waveform harmonic modes and orbital eccentricity. Furthermore, while the models are calibrated to agree with waveforms obtained by full numerical solutions of Einstein's equations, any such calibration is accurate only to some non-zero tolerance and is limited by the accuracy of the underlying phenomenology, availability, quality, and parameter-space coverage of numerical simulations. This paper complements the original analyses of GW150914 with an investigation of the effects of possible systematic errors in the waveform models on estimates of its source parameters. To test for systematic errors we repeat the original Bayesian analysis on mock signals from numerical simulations of a series of binary configurations with parameters similar to those found for GW150914. Overall, we find no evidence for a systematic bias relative to the statistical error of the original parameter recovery of GW150914 due to modeling approximations or modeling inaccuracies. However, parameter biases are found to occur for some configurations disfavored by the data of GW150914: for binaries inclined edge-on to the detector over a small range of choices of polarization angles, and also for eccentricities greater than\u2009\u2009~0.05. For signals with higher signal-to-noise ratio than GW150914, or in other regions of the binary parameter space (lower masses, larger mass ratios, or higher spins), we expect that systematic errors in current waveform models may impact gravitational-wave measurements, making more accurate models desirable for future observations.", "date": "2017-05-18", "date_type": "published", "publication": "Classical and Quantum Gravity", "volume": "34", "number": "10", "publisher": "IOP", "pagerange": "Art. No. 104002", "id_number": "CaltechAUTHORS:20170412-125626809", "issn": "0264-9381", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170412-125626809", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "Max Planck Society" }, { "agency": "State of Niedersachsen/Germany" }, { "agency": "Australian Research Council" }, { "agency": "Istituto Nazionale di Fisica Nucleare (INFN)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Stichting voor Fundamenteel Onderzoek der Materie (FOM)" }, { "agency": "Council of Scientific and Industrial Research (India)" }, { "agency": "Department of Science and Technology (India)" }, { "agency": "Science and Engineering Research Board (SERB)" }, { "agency": "Ministry of Human Resource Development (India)" }, { "agency": "Ministerio de Econom\u00eda y Competitividad (MINECO)" }, { "agency": "Conselleria d'Economia i Competitivitat and Conselleria d'Educaci\u00f3" }, { "agency": "Cultura i Universitats of the Govern de les Illes Balears" }, { "agency": "National Science Centre (Poland)" }, { "agency": "European Commission" }, { "agency": "Royal Society" }, { "agency": "Scottish Funding Council" }, { "agency": "Scottish Universities Physics Alliance" }, { "agency": "Hungarian Scientific Research Fund (OTKA)" }, { "agency": "Lyon Institute of Origins (LIO)" }, { "agency": "National Research Foundation of Korea" }, { "agency": "Industry Canada" }, { "agency": "Natural Science and Engineering Research Council of Canada (NSERC)" }, { "agency": "Canadian Institute for Advanced Research (CIFAR)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia, Inova\u00e7\u00e3o e Comunica\u00e7\u00e3o" }, { "agency": "Funda\u00e7\u00e3o de Amparo \u00e0 Pesquisa do Estado de S\u00e3o Paulo (FAPESP)" }, { "agency": "Russian Foundation for Basic Research" }, { "agency": "Leverhulme Trust" }, { "agency": "Research Corporation" }, { "agency": "Kavli Foundation" }, { "agency": "Ontario Ministry of Economic Development and Innovation" }, { "agency": "Ministry of Science and Technology (Taipei)" } ] }, "local_group": { "items": [ { "id": "LIGO" }, { "id": "Astronomy-Department" } ] }, "corp_creators": { "items": [ "LIGO Scientific Collaboration", "Virgo Collaboration" ] }, "doi": "10.1088/1361-6382/aa6854", "primary_object": { "basename": "1611.07531.pdf", "url": "https://authors.library.caltech.edu/records/zbkyq-2ye27/files/1611.07531.pdf" }, "resource_type": "article", "pub_year": "2017", "author_list": "Abbott, B. P.; Abbott, R.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/mq5jx-ya238", "eprint_id": 77016, "eprint_status": "archive", "datestamp": "2023-08-21 20:50:49", "lastmod": "2023-10-25 17:13:43", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kidder-L-E", "name": { "family": "Kidder", "given": "Lawrence E." }, "orcid": "0000-0001-5392-7342" }, { "id": "Field-S-E", "name": { "family": "Field", "given": "Scott E." } }, { "id": "Foucart-F", "name": { "family": "Foucart", "given": "Francois" }, "orcid": "0000-0003-4617-4738" }, { "id": "Schnetter-E", "name": { "family": "Schnetter", "given": "Erik" }, "orcid": "0000-0002-4518-9017" }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" }, { "id": "Bohn-A", "name": { "family": "Bohn", "given": "Andy" } }, { "id": "Deppe-N", "name": { "family": "Deppe", "given": "Nils" } }, { "id": "Diener-P", "name": { "family": "Diener", "given": "Peter" } }, { "id": "H\u00e9bert-F", "name": { "family": "H\u00e9bert", "given": "Fran\u00e7ois" } }, { "id": "Lippuner-J", "name": { "family": "Lippuner", "given": "Jonas" }, "orcid": "0000-0002-5936-3485" }, { "id": "Miller-J", "name": { "family": "Miller", "given": "Jonah" } }, { "id": "Ott-C-D", "name": { "family": "Ott", "given": "Christian D." }, "orcid": "0000-0003-4993-2055" }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." } }, { "id": "Vincent-T", "name": { "family": "Vincent", "given": "Trevor" } } ] }, "title": "SpECTRE: A task-based discontinuous Galerkin code for relativistic astrophysics", "ispublished": "pub", "full_text_status": "public", "keywords": "Discontinuous Galerkin; Hydrodynamics; Magnetohydrodynamics; Task-based parallelism", "note": "\u00a9 2017 Elsevier Inc. \n\nReceived 5 September 2016, Revised 21 December 2016, Accepted 29 December 2016, Available online 5 January 2017. \n\nWe acknowledge helpful discussions with Sebastiano Bernuzzi, Bernd Br\u00fcgmann, Marcus Bugner, Mani Chandra, Roland Haas, Daniel Hemberger, Jan Hesthaven, Cameron Hummels, Fraser Hutchison, Jonathan Lifflander, Geoffrey Lovelace, Phil Miller, Harald Pfeiffer, David Radice, and Christian Reisswig. We thank the anonymous referee for detailed comments and suggestions which helped to improve the manuscript. Support for F. Foucart was provided by NASA through Einstein Postdoctoral Fellowship grant numbered PF4-150122 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. Authors at Cornell were partially supported by NSF under award Nos. TCAN AST-1333129 and PHY-1306125, and by the Sherman Fairchild Foundation. Authors at Caltech were partially supported by NSF under award Nos. TCAN AST-1333520, CAREER PHY-1151197, and PHY-1404569, and by the Sherman Fairchild Foundation. ES acknowledges support from NSF award OCI-0905046. ES and JM were supported by an NSERC Discovery grant. Research at the Perimeter Institute is supported by the Government of Canada through Industry Canada and by the Province of Ontario through the Ministry of Research & Innovation. Computations were performed on NSF/NCSA Blue Waters under allocation PRAC ACI-1440083, on the NSF XSEDE network under allocations TG-PHY100033 and TG-PHY990007, and on the Caltech compute cluster Zwicky (NSF MRI-R2 award No. PHY-0960291).\n\nSubmitted - 1609.00098.pdf
", "abstract": "We introduce a new relativistic astrophysics code, SpECTRE, that combines a discontinuous Galerkin method with a task-based parallelism model. SpECTRE's goal is to achieve more accurate solutions for challenging relativistic astrophysics problems such as core-collapse supernovae and binary neutron star mergers. The robustness of the discontinuous Galerkin method allows for the use of high-resolution shock capturing methods in regions where (relativistic) shocks are found, while exploiting high-order accuracy in smooth regions. A task-based parallelism model allows efficient use of the largest supercomputers for problems with a heterogeneous workload over disparate spatial and temporal scales. We argue that the locality and algorithmic structure of discontinuous Galerkin methods will exhibit good scalability within a task-based parallelism framework. We demonstrate the code on a wide variety of challenging benchmark problems in (non)-relativistic (magneto)-hydrodynamics. We demonstrate the code's scalability including its strong scaling on the NCSA Blue Waters supercomputer up to the machine's full capacity of 22,380 nodes using 671,400 threads.", "date": "2017-04-15", "date_type": "published", "publication": "Journal of Computational Physics", "volume": "335", "publisher": "Elsevier", "pagerange": "84-114", "id_number": "CaltechAUTHORS:20170427-142549072", "issn": "0021-9991", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170427-142549072", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Einstein Fellowship", "grant_number": "PF4-150122" }, { "agency": "NASA", "grant_number": "NAS8-03060" }, { "agency": "NSF", "grant_number": "AST-1333129" }, { "agency": "NSF", "grant_number": "PHY-1306125" }, { "agency": "Sherman Fairchild Foundation" }, { "agency": "NSF", "grant_number": "AST-1333520" }, { "agency": "NSF", "grant_number": "PHY-1151197" }, { "agency": "NSF", "grant_number": "PHY-1404569" }, { "agency": "NSF", "grant_number": "OCI-0905046" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "Industry Canada" }, { "agency": "Ontario Ministry of Research and Innovation" }, { "agency": "NSF", "grant_number": "PRAC ACI-1440083" }, { "agency": "NSF", "grant_number": "TG-PHY100033" }, { "agency": "NSF", "grant_number": "TG-PHY990007N" }, { "agency": "NSF", "grant_number": "PHY-0960291" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.1016/j.jcp.2016.12.059", "primary_object": { "basename": "1609.00098.pdf", "url": "https://authors.library.caltech.edu/records/mq5jx-ya238/files/1609.00098.pdf" }, "resource_type": "article", "pub_year": "2017", "author_list": "Kidder, Lawrence E.; Field, Scott E.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/vsf0z-k4n51", "eprint_id": 72159, "eprint_status": "archive", "datestamp": "2023-08-19 00:38:09", "lastmod": "2023-10-23 17:59:31", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Lovelace-Geoffrey", "name": { "family": "Lovelace", "given": "Geoffrey" }, "orcid": "0000-0002-7084-1070" }, { "id": "Lousto-Carlos-O", "name": { "family": "Lousto", "given": "Carlos O." } }, { "id": "Healy-James", "name": { "family": "Healy", "given": "James" } }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." }, "orcid": "0000-0001-6656-9134" }, { "id": "Garcia-Alyssa", "name": { "family": "Garcia", "given": "Alyssa" } }, { "id": "O'Shaughnessy-Richard", "name": { "family": "O'Shaughnessy", "given": "Richard" }, "orcid": "0000-0001-5832-8517" }, { "id": "Boyle-Michael", "name": { "family": "Boyle", "given": "Michael" }, "orcid": "0000-0002-5075-5116" }, { "id": "Campanelli-Manuela", "name": { "family": "Campanelli", "given": "Manuela" } }, { "id": "Hemberger-Daniel-A", "name": { "family": "Hemberger", "given": "Daniel A." } }, { "id": "Kidder-Lawrence-E", "name": { "family": "Kidder", "given": "Lawrence E." }, "orcid": "0000-0001-5392-7342" }, { "id": "Pfeiffer-Harald-P", "name": { "family": "Pfeiffer", "given": "Harald P." }, "orcid": "0000-0001-9288-519X" }, { "id": "Szil\u00e1gyi-B\u00e9la", "name": { "family": "Szil\u00e1gyi", "given": "B\u00e9la" }, "orcid": "0000-0001-7744-6180" }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" }, { "id": "Zlochower-Y", "name": { "family": "Zlochower", "given": "Yosef" } } ] }, "title": "Modeling the source of GW150914 with targeted numerical-relativity simulations", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2016 IOP Publishing Ltd. \n\nReceived 18 July 2016. Accepted 28 October 2016. Published 18 November 2016. \n\nWe are pleased to acknowledge Joshua R Smith and Jocelyn S Read for helpful discussions of this work and Patricia Schmidt for helpful discussions and for helping us to implement the numerical-relativity injection HDF5 file format [113] she developed with Ian Harry, which facilitated some of the comparisons in this paper. We gratefully acknowledge the NSF for financial support from grant Nos. PHY-0969855, PHY-1212426, PHY-1305730, PHY-1306125, PHY-1307489, PHY-1229173, PHY-1404569, PHY-1606522, PHY-1607520, ACI-1550436, AST-1028087, AST-1333129, AST-1333520, OCI-0832606, and DRL-1136221. The authors are also grateful for support from the Louis Stokes Alliance for Minority Participation, which is supported by NSF grant No. HRD-1302873 and the California State University campuses and Office of the Chancellor, and for support from the Sherman Fairchild Foundation, the NSERC of Canada, the Canada Research Chairs Program, and the Canadian Institute for Advanced Research. Computational resources were provided by the ORCA cluster at California State University, Fullerton (CSUF), supported by CSUF, NSF grant No. PHY-1429873, and the Research Corporation for Science Advancement; by XSEDE allocations TG-PHY060027N and TG-PHY990007N; by NewHorizons and BlueSky Clusters at Rochester Institute of Technology, which were supported by NSF grant Nos. PHY-0722703, DMS-0820923, AST-1028087, and PHY-1229173; by the GPC supercomputer at the SciNet HPC Consortium [114], which is funded by the Canada Foundation for Innovation (CFI) under the auspices of Compute Canada, the Government of Ontario, the Ontario Research Fund (ORF)\u2014Research Excellence, and the University of Toronto; and by the Zwicky cluster at Caltech, which is supported by the Sherman Fairchild Foundation and by NSF award PHY-0960291.\n\nSubmitted - 1607.05377v1.pdf
", "abstract": "In fall of 2015, the two LIGO detectors measured the gravitational wave signal GW150914, which originated from a pair of merging black holes (Abbott et al Virgo, LIGO Scientific 2016 Phys. Rev. Lett. 116 061102). In the final 0.2\u2009s (about 8 gravitational-wave cycles) before the amplitude reached its maximum, the observed signal swept up in amplitude and frequency, from 35 Hz to 150 Hz. The theoretical gravitational-wave signal for merging black holes, as predicted by general relativity, can be computed only by full numerical relativity, because analytic approximations fail near the time of merger. Moreover, the nearly-equal masses, moderate spins, and small number of orbits of GW150914 are especially straightforward and efficient to simulate with modern numerical-relativity codes. In this paper, we report the modeling of GW150914 with numerical-relativity simulations, using black-hole masses and spins consistent with those inferred from LIGO's measurement (Abbott et al LIGO Scientific Collaboration, Virgo Collaboration 2016 Phys. Rev. Lett. 116 241102). In particular, we employ two independent numerical-relativity codes that use completely different analytical and numerical methods to model the same merging black holes and to compute the emitted gravitational waveform; we find excellent agreement between the waveforms produced by the two independent codes. These results demonstrate the validity, impact, and potential of current and future studies using rapid-response, targeted numerical-relativity simulations for better understanding gravitational-wave observations.", "date": "2016-12-22", "date_type": "published", "publication": "Classical and Quantum Gravity", "volume": "33", "number": "24", "publisher": "IOP", "pagerange": "Art. No. 244002", "id_number": "CaltechAUTHORS:20161118-110758994", "issn": "0264-9381", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161118-110758994", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY-0969855" }, { "agency": "NSF", "grant_number": "PHY-1212426" }, { "agency": "NSF", "grant_number": "PHY-1305730" }, { "agency": "NSF", "grant_number": "PHY-1306125" }, { "agency": "NSF", "grant_number": "PHY-1307489" }, { "agency": "NSF", "grant_number": "PHY-1229173" }, { "agency": "NSF", "grant_number": "PHY-1404569" }, { "agency": "NSF", "grant_number": "PHY-1606522" }, { "agency": "NSF", "grant_number": "PHY-1607520" }, { "agency": "NSF", "grant_number": "ACI-1550436" }, { "agency": "NSF", "grant_number": "AST-1028087" }, { "agency": "NSF", "grant_number": "AST-1333129" }, { "agency": "NSF", "grant_number": "AST-1333520" }, { "agency": "NSF", "grant_number": "OCI-0832606" }, { "agency": "NSF", "grant_number": "DRL-1136221" }, { "agency": "NSF", "grant_number": "HRD-1302873" }, { "agency": "Sherman Fairchild Foundation" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "Canada Research Chairs Program" }, { "agency": "Canadian Institute for Advanced Research (CIFAR)" }, { "agency": "NSF", "grant_number": "PHY-1429873" }, { "agency": "California State University, Fullerton" }, { "agency": "Research Corporation" }, { "agency": "NSF", "grant_number": "TG-PHY060027N" }, { "agency": "NSF", "grant_number": "TG-PHY990007N" }, { "agency": "NSF", "grant_number": "PHY-0722703" }, { "agency": "NSF", "grant_number": "DMS-0820923" }, { "agency": "NSF", "grant_number": "AST-1028087" }, { "agency": "NSF", "grant_number": "PHY-1229173" }, { "agency": "Canada Foundation for Innovation" }, { "agency": "Compute Canada" }, { "agency": "Ontario Research Fund-Research Excellence" }, { "agency": "University of Toronto" }, { "agency": "Caltech" }, { "agency": "NSF", "grant_number": "PHY-0960291" } ] }, "collection": "CaltechAUTHORS", "local_group": { "items": [ { "id": "TAPIR", "value": "TAPIR" } ] }, "doi": "10.1088/0264-9381/33/24/244002", "primary_object": { "basename": "1607.05377v1.pdf", "url": "https://authors.library.caltech.edu/records/vsf0z-k4n51/files/1607.05377v1.pdf" }, "resource_type": "article", "pub_year": "2016", "author_list": "Lovelace, Geoffrey; Lousto, Carlos O.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/2meeg-04d09", "eprint_id": 71440, "eprint_status": "archive", "datestamp": "2023-08-20 14:02:44", "lastmod": "2023-10-23 15:46:15", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Abbott-B-P", "name": { "family": "Abbott", "given": "B. P." } }, { "id": "Abbott-R", "name": { "family": "Abbott", "given": "R." } }, { "id": "Adhikari-R-X", "name": { "family": "Adhikari", "given": "R. X." }, "orcid": "0000-0002-5731-5076" }, { "id": "Anderson-S-B", "name": { "family": "Anderson", "given": "S. B." } }, { "id": "Arai-Koji", "name": { "family": "Arai", "given": "K." }, "orcid": "0000-0001-8916-8915" }, { "id": "Araya-M-C", "name": { "family": "Araya", "given": "M. C." } }, { "id": "Barayoga-J-C", "name": { "family": "Barayoga", "given": "J. C." } }, { "id": "Barish-B-C", "name": { "family": "Barish", "given": "B. C." } }, { "id": "Berger-B-K", "name": { "family": "Berger", "given": "B. K." } }, { "id": "Billingsley-G", "name": { "family": "Billingsley", "given": "G." }, "orcid": "0000-0002-4141-2744" }, { "id": "Blackburn-J-K", "name": { "family": "Blackburn", "given": "J. K." }, "orcid": "0000-0002-3838-2986" }, { "id": "Bork-R", "name": { "family": "Bork", "given": "R." } }, { "id": "Brooks-A-F", "name": { "family": "Brooks", "given": "A. F." }, "orcid": "0000-0003-4295-792X" }, { "id": "Brunett-S", "name": { "family": "Brunett", "given": "S." } }, { "id": "Cahillane-C", "name": { "family": "Cahillane", "given": "C." } }, { "id": "Callister-T-A", "name": { "family": "Callister", "given": "T." }, "orcid": "0000-0001-9892-177X" }, { "id": "Cepeda-C-B", "name": { "family": "Cepeda", "given": "C. B." } }, { "id": "Couvares-P", "name": { "family": "Couvares", "given": "P." } }, { "id": "Coyne-D-C", "name": { "family": "Coyne", "given": "D. C." }, "orcid": "0000-0002-6427-3222" }, { "id": "Dergachev-V", "name": { "family": "Dergachev", "given": "V." } }, { "id": "Drever-R-W-P", "name": { "family": "Drever", "given": "R. W. P." } }, { "id": "Ehrens-P", "name": { "family": "Ehrens", "given": "P." } }, { "id": "Etzel-T", "name": { "family": "Etzel", "given": "T." } }, { "id": "Gossan-S-E", "name": { "family": "Gossan", "given": "S. E." }, "orcid": "0000-0002-8138-9198" }, { "id": "Gushwa-K-E", "name": { "family": "Gushwa", "given": "K. E." } }, { "id": "Gustafson-E-K", "name": { "family": "Gustafson", "given": "E. K." } }, { "id": "Hall-E-D", "name": { "family": "Hall", "given": "E. D." }, "orcid": "0000-0001-9018-666X" }, { "id": "Heptonstall-A-W", "name": { "family": "Heptonstall", "given": "A. W." } }, { "id": "Isi-M", "name": { "family": "Isi", "given": "M." }, "orcid": "0000-0001-8830-8672" }, { "id": "Kanner-J-B", "name": { "family": "Kanner", "given": "J. B." }, "orcid": "0000-0001-8115-0577" }, { "id": "Kells-W", "name": { "family": "Kells", "given": "W." } }, { "id": "Kondrashov-V", "name": { "family": "Kondrashov", "given": "V." } }, { "id": "Korth-W-Z", "name": { "family": "Korth", "given": "W. Z." }, "orcid": "0000-0003-3527-1348" }, { "id": "Kozak-D-B", "name": { "family": "Kozak", "given": "D. B." }, "orcid": "0000-0003-3118-8950" }, { "id": "Lazzarini-A", "name": { "family": "Lazzarini", "given": "A." } }, { "id": "Lewis-J-B", "name": { "family": "Lewis", "given": "J. B." } }, { "id": "Maros-E", "name": { "family": "Maros", "given": "E." } }, { "id": "Marx-J-N", "name": { "family": "Marx", "given": "J. N." } }, { "id": "McIntyre-G", "name": { "family": "McIntyre", "given": "G." } }, { "id": "McIver-J", "name": { "family": "McIver", "given": "J." }, "orcid": "0000-0003-0316-1355" }, { "id": "Meshkov-S", "name": { "family": "Meshkov", "given": "S." } }, { "id": "Pedraza-M", "name": { "family": "Pedraza", "given": "M." } }, { "id": "Perreca-A", "name": { "family": "Perreca", "given": "A." } }, { "id": "Price-L-R", "name": { "family": "Price", "given": "L. R." } }, { "id": "Quintero-E-A", "name": { "family": "Quintero", "given": "E. A." } }, { "id": "Robertson-N-A", "name": { "family": "Robertson", "given": "N. A." } }, { "id": "Rollins-J-G", "name": { "family": "Rollins", "given": "J. G." } }, { "id": "Sachdev-S", "name": { "family": "Sachdev", "given": "S." }, "orcid": "0000-0002-2432-7070" }, { "id": "Sanchez-E-J", "name": { "family": "Sanchez", "given": "E. J." } }, { "id": "Schmidt-P", "name": { "family": "Schmidt", "given": "P." } }, { "id": "Singer-A", "name": { "family": "Singer", "given": "A." } }, { "id": "Smith-N-D", "name": { "family": "Smith", "given": "N. D." } }, { "id": "Smith-R-J-E", "name": { "family": "Smith", "given": "R. J. E." } }, { "id": "Taylor-R", "name": { "family": "Taylor", "given": "R." } }, { "id": "Thirugnanasambandam-M-P", "name": { "family": "Thirugnanasambandam", "given": "M. P." } }, { "id": "Torrie-C-I", "name": { "family": "Torrie", "given": "C. I." } }, { "id": "Vajente-G", "name": { "family": "Vajente", "given": "G." }, "orcid": "0000-0002-7656-6882" }, { "id": "Vass-S", "name": { "family": "Vass", "given": "S." } }, { "id": "Wallace-L", "name": { "family": "Wallace", "given": "L." } }, { "id": "Weinstein-Alan-J-Physics", "name": { "family": "Weinstein", "given": "A. J." }, "orcid": "0000-0002-0928-6784" }, { "id": "Williams-R-D", "name": { "family": "Williams", "given": "R. D." }, "orcid": "0000-0002-9145-8580" }, { "id": "Wipf-C-C", "name": { "family": "Wipf", "given": "C. C." } }, { "id": "Yamamoto-Hiroaki", "name": { "family": "Yamamoto", "given": "H." } }, { "id": "Zhang-Liyuan", "name": { "family": "Zhang", "given": "L." }, "orcid": "0000-0002-0898-787X" }, { "id": "Zucker-M-E", "name": { "family": "Zucker", "given": "M. E." }, "orcid": "0000-0002-2544-1596" }, { "id": "Zweizig-J", "name": { "family": "Zweizig", "given": "J." }, "orcid": "0000-0002-1521-3397" }, { "id": "Chen-Yanbei", "name": { "family": "Chen", "given": "Y." }, "orcid": "0000-0002-9730-9463" }, { "id": "Engels-W", "name": { "family": "Engels", "given": "W." } }, { "id": "Hemberger-D-A", "name": { "family": "Hemberger", "given": "D." } }, { "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "K. S." } }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "M." } }, { "id": "Szil\u00e1gyi-B", "name": { "family": "Szil\u00e1gyi", "given": "B." } }, { "id": "Vallisneri-M", "name": { "family": "Vallisneri", "given": "M." }, "orcid": "0000-0002-4162-0033" }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "S." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Improved analysis of GW150914 using a fully spin-precessing waveform model", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2016 Published by the American Physical Society under the terms of the Creative Commons Attribution 3.0 License. Further distribution of this work must maintain attribution to the author(s) and the published article's title, journal citation, and DOI.\n\n\nReceived 4 June 2016; revised manuscript received 30 July 2016; published 21 October 2016.\n\nThe authors gratefully acknowledge the support of the United States National Science Foundation (NSF) for the construction and operation of the LIGO Laboratory and Advanced LIGO, as well as the Science and Technology Facilities Council (STFC) of the United Kingdom, the Max-Planck Society (MPS), and the State of Niedersachsen/Germany for support of the construction of Advanced LIGO and construction and operation of the GEO600 detector. Additional support for Advanced LIGO was provided by the Australian Research Council. The authors gratefully acknowledge the Italian Istituto Nazionale di Fisica Nucleare (INFN), the French Centre National de la Recherche Scientifique (CNRS) and the Foundation for Fundamental Research on Matter supported by the Netherlands Organisation for Scientific Research, for the construction and operation of the Virgo detector and the creation and support of the EGO consortium. The authors also gratefully acknowledge research support from these agencies, as well as by the Council of Scientific and Industrial Research of India; Department of Science and Technology, India; Science & Engineering Research Board (SERB), India; Ministry of Human Resource Development, India; the Spanish Ministerio de Econom\u00eda y Competitividad; the Conselleria d'Economia i Competitivitat and Conselleria d'Educaci\u00f3; Cultura i Universitats of the Govern de les Illes Balears; the National Science Centre of Poland; the European Commission; the Royal Society; the Scottish Funding Council; the Scottish Universities Physics Alliance; the Hungarian Scientific Research Fund (OTKA); the Lyon Institute of Origins (LIO); the National Research Foundation of Korea; Industry Canada and the Province of Ontario through the Ministry of Economic Development and Innovation; the Natural Science and Engineering Research Council Canada; Canadian Institute for Advanced Research; the Brazilian Ministry of Science, Technology, and Innovation; Russian Foundation for Basic Research; the Leverhulme Trust; the Research Corporation; Ministry of Science and Technology (MOST), Taiwan; and the Kavli Foundation. The authors gratefully acknowledge the support of the NSF, STFC, MPS, INFN, CNRS, and the State of Niedersachsen/Germany for provision of computational resources.\n\nPublished - PhysRevX.6.041014.pdf
Submitted - 1606.01210v1.pdf
", "abstract": "This paper presents updated estimates of source parameters for GW150914, a binary black-hole coalescence event detected by the Laser Interferometer Gravitational-wave Observatory (LIGO) in 2015 [Abbott et al. Phys. Rev. Lett. 116, 061102 (2016).]. Abbott et al. [Phys. Rev. Lett. 116, 241102 (2016).] presented parameter estimation of the source using a 13-dimensional, phenomenological precessing-spin model (precessing IMRPhenom) and an 11-dimensional nonprecessing effective-one-body (EOB) model calibrated to numerical-relativity simulations, which forces spin alignment (nonprecessing EOBNR). Here, we present new results that include a 15-dimensional precessing-spin waveform model (precessing EOBNR) developed within the EOB formalism. We find good agreement with the parameters estimated previously [Abbott et al. Phys. Rev. Lett. 116, 241102 (2016).], and we quote updated component masses of 35^(+5)_(\u22123) M\u2299 and 30^(+3)_(\u22124) M\u2299 (where errors correspond to 90% symmetric credible intervals). We also present slightly tighter constraints on the dimensionless spin magnitudes of the two black holes, with a primary spin estimate <0.65 and a secondary spin estimate <0.75 at 90% probability. Abbott et al. [Phys. Rev. Lett. 116, 241102 (2016).] estimated the systematic parameter-extraction errors due to waveform-model uncertainty by combining the posterior probability densities of precessing IMRPhenom and nonprecessing EOBNR. Here, we find that the two precessing-spin models are in closer agreement, suggesting that these systematic errors are smaller than previously quoted.", "date": "2016-10", "date_type": "published", "publication": "Physical Review X", "volume": "6", "number": "4", "publisher": "American Physical Society", "pagerange": "Art. No. 041014", "id_number": "CaltechAUTHORS:20161025-090158516", "issn": "2160-3308", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161025-090158516", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "Max Planck Society" }, { "agency": "State of Niedersachsen/Germany" }, { "agency": "Australian Research Council" }, { "agency": "Istituto Nazionale di Fisica Nucleare (INFN)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Stichting voor Fundamenteel Onderzoek der Materie (FOM)" }, { "agency": "Council of Scientific and Industrial Research (India)" }, { "agency": "Department of Science and Technology (India)" }, { "agency": "Science & Engineering Research Board (SERB)" }, { "agency": "Ministry of Human Resource Development (India)" }, { "agency": "Ministerio de Econom\u00eda y Competitividad (MINECO)" }, { "agency": "Conselleria d'Economia i Competitivitat" }, { "agency": "Conselleria d'Educaci\u03cc, Cultura i Universitats of the Govern de les Illes Balears" }, { "agency": "National Science Centre (Poland)" }, { "agency": "European Commission" }, { "agency": "Royal Society" }, { "agency": "Scottish Funding Council" }, { "agency": "Scottish Universities Physics Alliance" }, { "agency": "Hungarian Scientific Research Fund (OTKA)" }, { "agency": "Lyon Institute of Origins (LIO)" }, { "agency": "National Research Foundation of Korea" }, { "agency": "Industry Canada" }, { "agency": "Ontario Ministry of Economic Development and Innovation" }, { "agency": "Natural Science and Engineering Research Council of Canada (NSERC)" }, { "agency": "Canadian Institute for Advanced Research (CIFAR)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Inova\u00e7\u00e3o" }, { "agency": "Russian Foundation for Basic Research" }, { "agency": "Leverhulme Trust" }, { "agency": "Research Corporation" }, { "agency": "Ministry of Science and Technology (Taipei)" }, { "agency": "Kavli Foundation" } ] }, "local_group": { "items": [ { "id": "LIGO" } ] }, "corp_creators": { "items": [ "LIGO Scientific Collaboration", "Virgo Collaboration" ] }, "doi": "10.1103/PhysRevX.6.041014", "primary_object": { "basename": "1606.01210v1.pdf", "url": "https://authors.library.caltech.edu/records/2meeg-04d09/files/1606.01210v1.pdf" }, "related_objects": [ { "basename": "PhysRevX.6.041014.pdf", "url": "https://authors.library.caltech.edu/records/2meeg-04d09/files/PhysRevX.6.041014.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Abbott, B. P.; Abbott, R.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/q59q4-wm358", "eprint_id": 70660, "eprint_status": "archive", "datestamp": "2023-08-20 13:49:47", "lastmod": "2023-10-20 23:18:28", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Abbott-B-P", "name": { "family": "Abbott", "given": "B. P." } }, { "id": "Abbott-R", "name": { "family": "Abbott", "given": "R." } }, { "id": "Adhikari-R-X", "name": { "family": "Adhikari", "given": "R. X." }, "orcid": "0000-0002-5731-5076" }, { "id": "Anderson-S-B", "name": { "family": "Anderson", "given": "S. B." } }, { "id": "Anderson-W-G", "name": { "family": "Anderson", "given": "W. G." } }, { "id": "Arai-Koji", "name": { "family": "Arai", "given": "K." }, "orcid": "0000-0001-8916-8915" }, { "id": "Araya-M-C", "name": { "family": "Araya", "given": "M. C." } }, { "id": "Barayoga-J-C", "name": { "family": "Barayoga", "given": "J. C." } }, { "id": "Barish-B-C", "name": { "family": "Barish", "given": "B. C." } }, { "id": "Berger-B-K", "name": { "family": "Berger", "given": "B. K." } }, { "id": "Billingsley-G", "name": { "family": "Billingsley", "given": "G." }, "orcid": "0000-0002-4141-2744" }, { "id": "Blackburn-J-K", "name": { "family": "Blackburn", "given": "J. K." }, "orcid": "0000-0002-3838-2986" }, { "id": "Bork-R", "name": { "family": "Bork", "given": "R." } }, { "id": "Brooks-A-F", "name": { "family": "Brooks", "given": "A. F." }, "orcid": "0000-0003-4295-792X" }, { "id": "Brunett-S", "name": { "family": "Brunett", "given": "S." } }, { "id": "Cahillane-C", "name": { "family": "Cahillane", "given": "C." } }, { "id": "Callister-T-A", "name": { "family": "Callister", "given": "T." }, "orcid": "0000-0001-9892-177X" }, { "id": "Cepeda-C-B", "name": { "family": "Cepeda", "given": "C. B." } }, { "id": "Couvares-P", "name": { "family": "Couvares", "given": "P." } }, { "id": "Coyne-D-C", "name": { "family": "Coyne", "given": "D. C." }, "orcid": "0000-0002-6427-3222" }, { "id": "Dergachev-V", "name": { "family": "Dergachev", "given": "V." } }, { "id": "Drever-R-W-P", "name": { "family": "Drever", "given": "R. W. P." } }, { "id": "Ehrens-P", "name": { "family": "Ehrens", "given": "P." } }, { "id": "Eichholz-J", "name": { "family": "Eichholz", "given": "J." } }, { "id": "Etzel-T", "name": { "family": "Etzel", "given": "T." } }, { "id": "Gossan-S-E", "name": { "family": "Gossan", "given": "S. E." }, "orcid": "0000-0002-8138-9198" }, { "id": "Gushwa-K-E", "name": { "family": "Gushwa", "given": "K. E." } }, { "id": "Gustafson-E-K", "name": { "family": "Gustafson", "given": "E. K." } }, { "id": "Hall-E-D", "name": { "family": "Hall", "given": "E. D." }, "orcid": "0000-0001-9018-666X" }, { "id": "Heptonstall-A-W", "name": { "family": "Heptonstall", "given": "A. W." } }, { "id": "Isi-M", "name": { "family": "Isi", "given": "M." }, "orcid": "0000-0001-8830-8672" }, { "id": "Kanner-J-B", "name": { "family": "Kanner", "given": "J. B." }, "orcid": "0000-0001-8115-0577" }, { "id": "Kells-W", "name": { "family": "Kells", "given": "W." } }, { "id": "Kondrashov-V", "name": { "family": "Kondrashov", "given": "V." } }, { "id": "Korth-W-Z", "name": { "family": "Korth", "given": "W. Z." }, "orcid": "0000-0003-3527-1348" }, { "id": "Kozak-D-B", "name": { "family": "Kozak", "given": "D. B." }, "orcid": "0000-0003-3118-8950" }, { "id": "Lazzarini-A", "name": { "family": "Lazzarini", "given": "A." } }, { "id": "Lewis-J-B", "name": { "family": "Lewis", "given": "J. B." } }, { "id": "Maros-E", "name": { "family": "Maros", "given": "E." } }, { "id": "Marx-J-N", "name": { "family": "Marx", "given": "J. N." } }, { "id": "McIntyre-G", "name": { "family": "McIntyre", "given": "G." } }, { "id": "McIver-J", "name": { "family": "McIver", "given": "J." }, "orcid": "0000-0003-0316-1355" }, { "id": "Meshkov-S", "name": { "family": "Meshkov", "given": "S." } }, { "id": "Pedraza-M", "name": { "family": "Pedraza", "given": "M." } }, { "id": "Perreca-A", "name": { "family": "Perreca", "given": "A." } }, { "id": "Price-L-R", "name": { "family": "Price", "given": "L. R." } }, { "id": "Quintero-E-A", "name": { "family": "Quintero", "given": "E. A." } }, { "id": "Reitze-D-H", "name": { "family": "Reitze", "given": "D. H." } }, { "id": "Robertson-N-A", "name": { "family": "Robertson", "given": "N. A." } }, { "id": "Rollins-J-G", "name": { "family": "Rollins", "given": "J. G." } }, { "id": "Sachdev-S", "name": { "family": "Sachdev", "given": "S." }, "orcid": "0000-0002-2432-7070" }, { "id": "Sanchez-E-J", "name": { "family": "Sanchez", "given": "E. J." } }, { "id": "Schmidt-P", "name": { "family": "Schmidt", "given": "P." } }, { "id": "Singer-A", "name": { "family": "Singer", "given": "A." } }, { "id": "Smith-N-D", "name": { "family": "Smith", "given": "N. D." } }, { "id": "Smith-R-J-E", "name": { "family": "Smith", "given": "R. J. E." } }, { "id": "Taylor-R", "name": { "family": "Taylor", "given": "R." } }, { "id": "Thirugnanasambandam-M-P", "name": { "family": "Thirugnanasambandam", "given": "M. P." } }, { "id": "Torrie-C-I", "name": { "family": "Torrie", "given": "C. I." } }, { "id": "Vajente-G", "name": { "family": "Vajente", "given": "G." }, "orcid": "0000-0002-7656-6882" }, { "id": "Vass-S", "name": { "family": "Vass", "given": "S." } }, { "id": "Wallace-L", "name": { "family": "Wallace", "given": "L." } }, { "id": "Weinstein-Alan-J-Physics", "name": { "family": "Weinstein", "given": "A. J." }, "orcid": "0000-0002-0928-6784" }, { "id": "Williams-R-D", "name": { "family": "Williams", "given": "R. D." }, "orcid": "0000-0002-9145-8580" }, { "id": "Wipf-C-C", "name": { "family": "Wipf", "given": "C. C." } }, { "id": "Yamamoto-Hiroaki", "name": { "family": "Yamamoto", "given": "H." } }, { "id": "Zhang-Liyuan", "name": { "family": "Zhang", "given": "L." }, "orcid": "0000-0002-0898-787X" }, { "id": "Zucker-M-E", "name": { "family": "Zucker", "given": "M. E." }, "orcid": "0000-0002-2544-1596" }, { "id": "Zweizig-J", "name": { "family": "Zweizig", "given": "J." }, "orcid": "0000-0002-1521-3397" }, { "id": "Chen-Yanbei", "name": { "family": "Chen", "given": "Y." }, "orcid": "0000-0002-9730-9463" }, { "id": "Engels-W", "name": { "family": "Engels", "given": "W." } }, { "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "K. S." } }, { "id": "Hemberger-D-A", "name": { "family": "Hemberger", "given": "D." } }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "M." } }, { "id": "Szil\u00e1gyi-B", "name": { "family": "Szilagyi", "given": "B." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "S." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Directly comparing GW150914 with numerical solutions of Einstein's equations for binary black hole coalescence", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2016 American Physical Society. \n\nReceived 10 June 2016; published 14 September 2016. \n\nThe authors gratefully acknowledge helpful feedback from an anonymous referee. The authors gratefully acknowledge the support of the United States National Science Foundation (NSF) for the construction and operation of the LIGO Laboratory and Advanced LIGO as well as the Science and Technology Facilities Council (STFC) of the United Kingdom, the Max-Planck-Society (MPS), and the State of Niedersachsen/Germany for support of the construction of Advanced LIGO and construction and operation of the GEO600 detector. Additional support for Advanced LIGO was provided by the Australian Research Council. The authors gratefully acknowledge the Italian Istituto Nazionale di Fisica Nucleare (INFN), the French Centre National de la Recherche Scientifique (CNRS) and the Foundation for Fundamental Research on Matter supported by the Netherlands Organisation for Scientific Research, for the construction and operation of the Virgo detector and the creation and support of the EGO consortium. The authors also gratefully acknowledge research support from these agencies as well as by the Council of Scientific and Industrial Research of India, Department of Science and Technology, India, Science & Engineering Research Board (SERB), India, Ministry of Human Resource Development, India, the Spanish Ministerio de Econom\u00eda y Competitividad, the Conselleria d'Economia i Competitivitat and Conselleria d'Educaci\u00f3, Cultura i Universitats of the Govern de les Illes Balears, the National Science Centre of Poland, the European Commission, the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, the Hungarian Scientific Research Fund (OTKA), the Lyon Institute of Origins (LIO), the National Research Foundation of Korea, Industry Canada and the Province of Ontario through the Ministry of Economic Development and Innovation, the National Science and Engineering Research Council Canada, the Brazilian Ministry of Science, Technology, and Innovation, the Leverhulme Trust, the Research Corporation, Ministry of Science and Technology (MOST), Taiwan and the Kavli Foundation. The authors gratefully acknowledge the support of the NSF, STFC, MPS, INFN, CNRS, and the State of Niedersachsen/Germany for provision of computational resources. The SXS Collaboration also gratefully acknowledges Compute Canada, the Research Corporation, and California State University Fullerton for computational resources, as well as the support of the National Science Foundation, the Research Corporation for Science Advancement,and the Sherman Fairchild Foundation. The RIT team gratefully acknowledges the NSF for financial support, as well as Blue Waters and XSEDE for computational resources. This paper has been assigned the document number LIGO-P1500263.\n\nPublished - PhysRevD.94.064035.pdf
Submitted - 1606.01262v1.pdf
Supplemental Material - paper-tables-long.pdf
", "abstract": "We compare GW150914 directly to simulations of coalescing binary black holes in full general relativity, including several performed specifically to reproduce this event. Our calculations go beyond existing semianalytic models, because for all simulations\u2014including sources with two independent, precessing spins\u2014we perform comparisons which account for all the spin-weighted quadrupolar modes, and separately which account for all the quadrupolar and octopolar modes. Consistent with the posterior distributions reported by Abbott et al. [Phys. Rev. Lett. 116, 241102 (2016)] (at the 90% credible level), we find the data are compatible with a wide range of nonprecessing and precessing simulations. Follow-up simulations performed using previously estimated binary parameters most resemble the data, even when all quadrupolar and octopolar modes are included. Comparisons including only the quadrupolar modes constrain the total redshifted mass M_z \u2208[64\u2009\u2009M_\u2299\u221282\u2009\u2009M_\u2299], mass ratio 1/q = m_2/m_1 \u2208[0.6,1], and effective aligned spin \u03c7_(eff) \u2208[\u22120.3,0.2], where \u03c7_(eff)=(S_1/m_1+S_2/m_2)\u22c5L/M. Including both quadrupolar and octopolar modes, we find the mass ratio is even more tightly constrained. Even accounting for precession, simulations with extreme mass ratios and effective spins are highly inconsistent with the data, at any mass. Several nonprecessing and precessing simulations with similar mass ratio and \u03c7_(eff) are consistent with the data. Though correlated, the components' spins (both in magnitude and directions) are not significantly constrained by the data: the data is consistent with simulations with component spin magnitudes \u0251_(1,2) up to at least 0.8, with random orientations. Further detailed follow-up calculations are needed to determine if the data contain a weak imprint from transverse (precessing) spins. For nonprecessing binaries, interpolating between simulations, we reconstruct a posterior distribution consistent with previous results. The final black hole's redshifted mass is consistent with Mf,z in the range 64.0\u2009\u2009M_\u2299\u221273.5\u2009\u2009M_\u2299 and the final black hole's dimensionless spin parameter is consistent with \u0251_f = 0.62\u20130.73. As our approach invokes no intermediate approximations to general relativity and can strongly reject binaries whose radiation is inconsistent with the data, our analysis provides a valuable complement to Abbott et al. [Phys. Rev. Lett. 116, 241102 (2016)].", "date": "2016-09-15", "date_type": "published", "publication": "Physical Review D", "volume": "94", "number": "6", "publisher": "American Physical Society", "pagerange": "Art. No. 064035", "id_number": "CaltechAUTHORS:20160929-105317375", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160929-105317375", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "Max-Planck-Society" }, { "agency": "State of Niedersachsen/Germany" }, { "agency": "Australian Research Council" }, { "agency": "Istituto Nazionale di Fisica Nucleare (INFN)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Stichting voor Fundamenteel Onderzoek der Materie (FOM)" }, { "agency": "Council of Scientific and Industrial Research (India)" }, { "agency": "Department of Science and Technology (India)" }, { "agency": "Science and Engineering Research Board (SERB)" }, { "agency": "Ministry of Human Resource Development (India)" }, { "agency": "Ministerio de Econom\u00eda y Competitividad (MINECO)" }, { "agency": "Conselleria d'Economia i Competitivitat and Conselleria d'Educaci\u00f3" }, { "agency": "Cultura i Universitats of the Govern de les Illes Balears" }, { "agency": "National Science Centre (Poland)" }, { "agency": "European Commission" }, { "agency": "Royal Society" }, { "agency": "Scottish Funding Council" }, { "agency": "Scottish Universities Physics Alliance" }, { "agency": "Hungarian Scientific Research Fund (OTKA)" }, { "agency": "Lyon Institute of Origins (LIO)" }, { "agency": "National Research Foundation of Korea" }, { "agency": "Industry Canada" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Inova\u00e7\u00e3o" }, { "agency": "Leverhulme Trust" }, { "agency": "Research Corporation" }, { "agency": "Ministry of Science and Technology (Taipei)" }, { "agency": "Kavli Foundation" }, { "agency": "NSF" }, { "agency": "Ontario Ministry of Economic Development and Innovation" } ] }, "other_numbering_system": { "items": [ { "id": "P1500263", "name": "LIGO Document" } ] }, "local_group": { "items": [ { "id": "LIGO" }, { "id": "TAPIR" } ] }, "corp_creators": { "items": [ "LIGO Scientific Collaboration", "Virgo Collaboration" ] }, "doi": "10.1103/PhysRevD.94.064035", "primary_object": { "basename": "PhysRevD.94.064035.pdf", "url": "https://authors.library.caltech.edu/records/q59q4-wm358/files/PhysRevD.94.064035.pdf" }, "related_objects": [ { "basename": "paper-tables-long.pdf", "url": "https://authors.library.caltech.edu/records/q59q4-wm358/files/paper-tables-long.pdf" }, { "basename": "1606.01262v1.pdf", "url": "https://authors.library.caltech.edu/records/q59q4-wm358/files/1606.01262v1.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Abbott, B. P.; Abbott, R.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/ram0a-34x88", "eprint_id": 86814, "eprint_status": "archive", "datestamp": "2023-08-20 13:50:09", "lastmod": "2023-10-18 20:36:35", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bohn-A", "name": { "family": "Bohn", "given": "Andy" } }, { "id": "Kidder-L-E", "name": { "family": "Kidder", "given": "Lawrence E." }, "orcid": "0000-0001-5392-7342" }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Parallel adaptive event horizon finder for numerical relativity", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2016 American Physical Society. \n\n(Received 7 June 2016; published 2 September 2016) \n\nWe thank David Nichols for useful conversations about affine parametrizations of event horizon generators. We are grateful to Fran\u00e7ois H\u00e9bert and William Throwe for various helpful conversations including numerous triangle drawing whiteboard sessions. We thank Daniel A. Hemberger for helping us understand the intricacies of the adaptive mesh refinement in spec. For helping smooth the visualization of event horizon surfaces, we thank Curran D. Muhlberger. We also thank Harald Pfeiffer for providing the BBH simulation with parameters similar to the system detected by Advanced LIGO, shown in Fig. 11. For providing useful suggestions during the writing phase, we thank Nils Deppe. We gratefully acknowledge support for this research at Cornell from the Sherman Fairchild Foundation and NSF Grants No. PHY-1306125 and No. AST-1333129. Calculations were performed on the Zwicky cluster at Caltech, which is supported by the Sherman Fairchild Foundation and by NSF Grant No. PHY-0960291; on the NFS XSEDE network under Grant No. TG-PHY990007N; at the GPC supercomputer at the SciNet HPC Consortium [40] [SciNet is funded by the Canada Foundation for Innovation (CFI) under the auspices of Compute Canada]; the Government of Ontario; Ontario Research Fund (ORF)\u2014Research Excellence; and the University of Toronto. All the surface visualizations were done using Paraview [41].\n\nPublished - PhysRevD.94.064008.pdf
Submitted - 1606.00437
", "abstract": "With Advanced LIGO detecting the gravitational waves emitted from a pair of merging black holes in late 2015, we have a new perspective into the strong field regime of binary black hole systems. Event horizons are the defining features of such black hole spacetimes. We introduce a new code for locating event horizons in numerical simulations based on a Delaunay triangulation on a topological sphere. The code can automatically refine arbitrary regions of the event horizon surface to find and explore features such as the hole in a toroidal event horizon, as discussed in our companion paper. We also investigate various ways of integrating the geodesic equation and find evolution equations that can be integrated efficiently with high accuracy.", "date": "2016-09-15", "date_type": "published", "publication": "Physical Review D", "volume": "94", "number": "6", "publisher": "American Physical Society", "pagerange": "Art. No. 064008", "id_number": "CaltechAUTHORS:20180605-162854944", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180605-162854944", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Sherman Fairchild Foundation" }, { "agency": "NSF", "grant_number": "PHY-1306125" }, { "agency": "NSF", "grant_number": "AST-1333129" }, { "agency": "NSF", "grant_number": "PHY-0960291" }, { "agency": "NSF", "grant_number": "TG-PHY990007N" }, { "agency": "Canada Foundation for Innovation" }, { "agency": "Compute Canada" }, { "agency": "Government of Ontario" }, { "agency": "Ontario Research Fund-Research Excellence" }, { "agency": "University of Toronto" } ] }, "doi": "10.1103/PhysRevD.94.064008", "primary_object": { "basename": "1606.00437", "url": "https://authors.library.caltech.edu/records/ram0a-34x88/files/1606.00437" }, "related_objects": [ { "basename": "PhysRevD.94.064008.pdf", "url": "https://authors.library.caltech.edu/records/ram0a-34x88/files/PhysRevD.94.064008.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Bohn, Andy; Kidder, Lawrence E.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/1y5tn-xrx80", "eprint_id": 86813, "eprint_status": "archive", "datestamp": "2023-08-20 13:50:03", "lastmod": "2023-10-18 20:36:32", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bohn-A", "name": { "family": "Bohn", "given": "Andy" } }, { "id": "Kidder-L-E", "name": { "family": "Kidder", "given": "Lawrence E." }, "orcid": "0000-0001-5392-7342" }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Toroidal horizons in binary black hole mergers", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2016 American Physical Society. \n\n(Received 7 June 2016; published 2 September 2016) \n\nWe thank Aaron Zimmerman for the suggestion of using a negative amplitude Gaussian to create a baby event horizon and for helpful dialogue regarding topologies of event horizon surfaces. For ongoing feedback and suggestions for finding toroidal event horizons over the past few years, we thank Jeffrey Winicour. We also thank Michael Boyle for useful conversations about topologies of event horizon surfaces and useful paper comments. We thank Leo C. Stein for verifying the effects of coordinate transformations and useful paper comments. For keeping the SpEC code from changing under us while we were locating event horizons, we thank Daniel A. Hemberger. We are grateful to Jordan Moxon, Nils Deppe, and Fran\u00e7ois H\u00e9bert for time slicing conversations and useful comments during the editing phase of this paper. We also thank Harald Pfeiffer for providing the BBH simulation with parameters similar to the system detected by Advanced LIGO. For helping smooth the visualization of event horizon surfaces, we thank Curran D. Muhlberger. We gratefully acknowledge support for this research at Cornell from the Sherman Fairchild Foundation and NSF Grants No. PHY-1306125 and No. AST-1333129. Calculations were performed on the Zwicky cluster at Caltech, which is supported by the Sherman Fairchild Foundation and by NSF Grant No. PHY-0960291; on the NFS XSEDE network under Grant No. TG-PHY990007N; at the GPC supercomputer at the SciNet HPC Consortium [36]. SciNet is funded by the Canada Foundation for Innovation under the auspices of Compute Canada, the Government of Ontario, Ontario Research Fund Research Excellence, and the University of Toronto. All the surface visualizations were done using Paraview [37]. The line plots were produced using the Matplotlib [38] library with Python.\n\nPublished - PhysRevD.94.064009.pdf
Submitted - 1606.00436
", "abstract": "We find the first binary black hole event horizon with a toroidal topology. It has been predicted that generically the event horizons of merging black holes should briefly have a toroidal topology. However, such a phase has never been seen in numerical simulations. Instead, in all previous simulations, the topology of the event horizon transitions directly from two spheres during the inspiral to a single sphere as the black holes merge. We find a coordinate transformation to a foliation of spacelike hypersurfaces that \"cut a hole\" through the event horizon surface, resulting in a toroidal event horizon, thus reconciling the numerical work with theoretical expectations. The demonstration requires extremely high numerical precision, which is made possible by a new event horizon code described in a companion paper. A torus could potentially provide a mechanism for violating topological censorship. However, these toroidal event horizons satisfy topological censorship by construction, because we can always trivially apply the inverse coordinate transformation to remove the topological feature.", "date": "2016-09-15", "date_type": "published", "publication": "Physical Review D", "volume": "94", "number": "6", "publisher": "American Physical Society", "pagerange": "Art. No. 064009", "id_number": "CaltechAUTHORS:20180605-162330969", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180605-162330969", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Sherman Fairchild Foundation" }, { "agency": "NSF", "grant_number": "PHY-1306125" }, { "agency": "NSF", "grant_number": "AST-1333129" }, { "agency": "NSF", "grant_number": "PHY-0960291" }, { "agency": "NSF", "grant_number": "TG-PHY990007N" }, { "agency": "Canada Foundation for Innovation" }, { "agency": "Compute Canada" }, { "agency": "Government of Ontario" }, { "agency": "Ontario Research Fund-Research Excellence" }, { "agency": "University of Toronto" } ] }, "doi": "10.1103/PhysRevD.94.064009", "primary_object": { "basename": "1606.00436", "url": "https://authors.library.caltech.edu/records/1y5tn-xrx80/files/1606.00436" }, "related_objects": [ { "basename": "PhysRevD.94.064009.pdf", "url": "https://authors.library.caltech.edu/records/1y5tn-xrx80/files/PhysRevD.94.064009.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Bohn, Andy; Kidder, Lawrence E.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/9cyhc-mrt24", "eprint_id": 68695, "eprint_status": "archive", "datestamp": "2023-08-20 12:28:26", "lastmod": "2023-10-19 23:16:18", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Haas-R", "name": { "family": "Haas", "given": "Roland" }, "orcid": "0000-0003-1424-6178" }, { "id": "Ott-C-D", "name": { "family": "Ott", "given": "Christian D." }, "orcid": "0000-0003-4993-2055" }, { "id": "Szilagyi-B", "name": { "family": "Szilagyi", "given": "Bela" } }, { "id": "Kaplan-J-D", "name": { "family": "Kaplan", "given": "Jeffrey D." } }, { "id": "Lippuner-J", "name": { "family": "Lippuner", "given": "Jonas" }, "orcid": "0000-0002-5936-3485" }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." } }, { "id": "Barkett-K", "name": { "family": "Barkett", "given": "Kevin" } }, { "id": "Muhlberger-C-D", "name": { "family": "Muhlberger", "given": "Curran D." } }, { "id": "Dietrich-T", "name": { "family": "Dietrich", "given": "Tim" } }, { "id": "Duez-M-D", "name": { "family": "Duez", "given": "Matthew D." }, "orcid": "0000-0002-0050-1783" }, { "id": "Foucart-F", "name": { "family": "Foucart", "given": "Francois" }, "orcid": "0000-0003-4617-4738" }, { "id": "Pfeiffer-H-P", "name": { "family": "Pfeiffer", "given": "Harald P." }, "orcid": "0000-0001-9288-519X" }, { "id": "Kidder-L-E", "name": { "family": "Kidder", "given": "Lawrence E." }, "orcid": "0000-0001-5392-7342" }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Simulations of inspiraling and merging double neutron stars using the Spectral Einstein Code", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2016 American Physical Society. \n\nReceived 7 April 2016. Received 7 April 2016; published 24 June 2016.\n\nWe acknowledge helpful discussions with Sebastiano\nBernuzzi, Michael Boyle [123], Alessandra Buonanno, M.\nBrett Deaton, Sarah Gossan, Tanja Hinderer, Kenta Kiuchi,\nLuis Lehner, Geoffrey Lovelace, Maria Okounkova, David\nRadice, Jocelyn Read, Masaru Shibata, Nick Tacik, and\nmembers of our Simulating eXtreme Spacetimes (SXS)\ncollaboration (http://www.black\u2011holes.org). This research\nis partially supported by NSF Grants No. PHY-1068881,\nNo. CAREER PHY-1151197, No. PHY-1306125,\nNo. PHY-1404569, No. PHY-1402916, No. AST-\n1205732, No. AST-1333129, and No. AST-1333520; by\nthe Alfred P. Sloan Foundation; by the Max-Planck\nSociety; by the Sherman Fairchild Foundation; and by\nthe International Research Unit of Advanced Future\nStudies, Kyoto University. Support for F. F. was provided\nby NASA through Einstein Postdoctoral Fellowship Grant\nNo. PF4-150122 awarded by the Chandra X-ray Center,\nwhich is operated by the Smithsonian Astrophysical\nObservatory for NASA under Contract No. NAS8-\n03060. The simulations were performed on the Caltech\ncompute cluster Zwicky (NSF MRI Grant No. PHY-\n0960291), on the Datura cluster of the AEI, on machines\nof the Louisiana Optical Network Initiative under Grant\nNo. loni_numrel07, and on Stampede at TACC under\nNSF XSEDE allocations No. TG-PHY990007N and No. TG-PHY100033. All 2D graphs were generated with\nthe PYTHON-based MATPLOTLIB [124] and IPYTHON [125]\npackages. VISIT [126,127] was used for 3D and 2D sliced\nplots. This paper has been assigned Yukawa Institute for\nTheoretical Physics Report No. YITP-16-39.\n\nPublished - PhysRevD.93.124062.pdf
Submitted - 1604.00782v1.pdf
", "abstract": "We present results on the inspiral, merger, and postmerger evolution of a neutron star-neutron star (NSNS) system. Our results are obtained using the hybrid pseudospectral-finite volume Spectral Einstein Code (SpEC). To test our numerical methods, we evolve an equal-mass system for \u224822 orbits before merger. This waveform is the longest waveform obtained from fully general-relativistic simulations for NSNSs to date. Such long (and accurate) numerical waveforms are required to further improve semianalytical models used in gravitational wave data analysis, for example, the effective one body models. We discuss in detail the improvements to SpEC's ability to simulate NSNS mergers, in particular mesh refined grids to better resolve the merger and postmerger phases. We provide a set of consistency checks and compare our results to NSNS merger simulations with the independent bam code. We find agreement between them, which increases confidence in results obtained with either code. This work paves the way for future studies using long waveforms and more complex microphysical descriptions of neutron star matter in SpEC.", "date": "2016-06-24", "date_type": "published", "publication": "Physical Review D", "volume": "93", "number": "12", "publisher": "American Physical Society", "pagerange": "Art. No. 124062", "id_number": "CaltechAUTHORS:20160627-150704335", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160627-150704335", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY-1068881" }, { "agency": "NSF CAREER", "grant_number": "PHY-1151197" }, { "agency": "NSF", "grant_number": "PHY-1306125" }, { "agency": "NSF", "grant_number": "PHY-1404569" }, { "agency": "NSF", "grant_number": "PHY-1402916" }, { "agency": "NSF", "grant_number": "AST- 1205732" }, { "agency": "NSF", "grant_number": "AST-1333129" }, { "agency": "NSF", "grant_number": "AST-1333520" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "Max-Planck Society" }, { "agency": "Sherman Fairchild Foundation" }, { "agency": "International Research Unit of Advanced Future Studies" }, { "agency": "Kyoto University" }, { "agency": "NASA Einstein Postdoctoral Fellowship", "grant_number": "PF4-150122" }, { "agency": "NASA", "grant_number": "NAS8- 03060" }, { "agency": "NSF MRI", "grant_number": "PHY- 0960291" }, { "agency": "Louisiana Optical Network Initiative", "grant_number": "loni_numrel07" }, { "agency": "NSF XSEDE", "grant_number": "TG-PHY990007N" }, { "agency": "NSF XSEDE", "grant_number": "TG-PHY100033" } ] }, "local_group": { "items": [ { "id": "TAPIR" } ] }, "doi": "10.1103/PhysRevD.93.124062", "primary_object": { "basename": "1604.00782v1.pdf", "url": "https://authors.library.caltech.edu/records/9cyhc-mrt24/files/1604.00782v1.pdf" }, "related_objects": [ { "basename": "PhysRevD.93.124062.pdf", "url": "https://authors.library.caltech.edu/records/9cyhc-mrt24/files/PhysRevD.93.124062.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Haas, Roland; Ott, Christian D.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/mt5ym-r8015", "eprint_id": 67967, "eprint_status": "archive", "datestamp": "2023-08-20 12:24:18", "lastmod": "2023-10-19 22:09:06", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Abbott-B-P", "name": { "family": "Abbott", "given": "B. P." } }, { "id": "Abbott-R", "name": { "family": "Abbott", "given": "R." } }, { "id": "Abernathy-M-R", "name": { "family": "Abernathy", "given": "M. R." } }, { "id": "Adhikari-R-X", "name": { "family": "Adhikari", "given": "R. X." }, "orcid": "0000-0002-5731-5076" }, { "id": "Anderson-S-B", "name": { "family": "Anderson", "given": "S. B." } }, { "id": "Arai-Koji", "name": { "family": "Arai", "given": "K." }, "orcid": "0000-0001-8916-8915" }, { "id": "Araya-M-C", "name": { "family": "Araya", "given": "M. C." } }, { "id": "Barayoga-J-C", "name": { "family": "Barayoga", "given": "J. C." } }, { "id": "Barish-B-C", "name": { "family": "Barish", "given": "B. C." } }, { "id": "Berger-B-K", "name": { "family": "Berger", "given": "B. K." } }, { "id": "Billingsley-G", "name": { "family": "Billingsley", "given": "G." }, "orcid": "0000-0002-4141-2744" }, { "id": "Blackburn-J-K", "name": { "family": "Blackburn", "given": "J. K." }, "orcid": "0000-0002-3838-2986" }, { "id": "Bork-R", "name": { "family": "Bork", "given": "R." } }, { "id": "Brooks-A-F", "name": { "family": "Brooks", "given": "A. F." }, "orcid": "0000-0003-4295-792X" }, { "id": "Cahillane-C", "name": { "family": "Cahillane", "given": "C." } }, { "id": "Callister-T-A", "name": { "family": "Callister", "given": "T." }, "orcid": "0000-0001-9892-177X" }, { "id": "Cepeda-C-B", "name": { "family": "Cepeda", "given": "C. B." } }, { "id": "Chakraborty-R", "name": { "family": "Chakraborty", "given": "R." } }, { "id": "Chalermsongsak-T", "name": { "family": "Chalermsongsak", "given": "T." } }, { "id": "Couvares-P", "name": { "family": "Couvares", "given": "P." } }, { "id": "Coyne-D-C", "name": { "family": "Coyne", "given": "D. C." }, "orcid": "0000-0002-6427-3222" }, { "id": "Dergachev-V", "name": { "family": "Dergachev", "given": "V." } }, { "id": "Drever-R-W-P", "name": { "family": "Drever", "given": "R. W. P." } }, { "id": "Ehrens-P", "name": { "family": "Ehrens", "given": "P." } }, { "id": "Etzel-T", "name": { "family": "Etzel", "given": "T." } }, { "id": "Gossan-S-E", "name": { "family": "Gossan", "given": "S. E." }, "orcid": "0000-0002-8138-9198" }, { "id": "Gushwa-K-E", "name": { "family": "Gushwa", "given": "K. E." } }, { "id": "Gustafson-E-K", "name": { "family": "Gustafson", "given": "E. K." } }, { "id": "Hall-E-D", "name": { "family": "Hall", "given": "E. D." }, "orcid": "0000-0001-9018-666X" }, { "id": "Heptonstall-A-W", "name": { "family": "Heptonstall", "given": "A. W." } }, { "id": "Hodge-K-A", "name": { "family": "Hodge", "given": "K. A." } }, { "id": "Isi-M", "name": { "family": "Isi", "given": "M." }, "orcid": "0000-0001-8830-8672" }, { "id": "Kanner-J-B", "name": { "family": "Kanner", "given": "J. B." }, "orcid": "0000-0001-8115-0577" }, { "id": "Kells-W", "name": { "family": "Kells", "given": "W." } }, { "id": "Kondrashov-V", "name": { "family": "Kondrashov", "given": "V." } }, { "id": "Korth-W-Z", "name": { "family": "Korth", "given": "W. Z." }, "orcid": "0000-0003-3527-1348" }, { "id": "Kozak-D-B", "name": { "family": "Kozak", "given": "D. B." }, "orcid": "0000-0003-3118-8950" }, { "id": "Lazzarini-A", "name": { "family": "Lazzarini", "given": "A." } }, { "id": "Li-T-G-F", "name": { "family": "Li", "given": "T. G. F." } }, { "id": "Mageswaran-M", "name": { "family": "Mageswaran", "given": "M." } }, { "id": "Maros-E", "name": { "family": "Maros", "given": "E." } }, { "id": "Martynov-D-V", "name": { "family": "Martynov", "given": "D. V." } }, { "id": "Marx-J-N", "name": { "family": "Marx", "given": "J. N." } }, { "id": "McIntyre-G", "name": { "family": "McIntyre", "given": "G." } }, { "id": "McIver-J", "name": { "family": "McIver", "given": "J." }, "orcid": "0000-0003-0316-1355" }, { "id": "Meshkov-S", "name": { "family": "Meshkov", "given": "S." } }, { "id": "Pedraza-M", "name": { "family": "Pedraza", "given": "M." } }, { "id": "Perreca-A", "name": { "family": "Perreca", "given": "A." } }, { "id": "Price-L-R", "name": { "family": "Price", "given": "L. R." } }, { "id": "Quintero-E-A", "name": { "family": "Quintero", "given": "E. A." } }, { "id": "Reitze-D-H", "name": { "family": "Reitze", "given": "D. H." } }, { "id": "Robertson-N-A", "name": { "family": "Robertson", "given": "N. A." } }, { "id": "Rollins-J-G", "name": { "family": "Rollins", "given": "J. G." } }, { "id": "Sachdev-S", "name": { "family": "Sachdev", "given": "S." }, "orcid": "0000-0002-2432-7070" }, { "id": "Sanchez-E-J", "name": { "family": "Sanchez", "given": "E. J." } }, { "id": "Schmidt-P", "name": { "family": "Schmidt", "given": "P." } }, { "id": "Shao-Z", "name": { "family": "Shao", "given": "Z." } }, { "id": "Singer-A", "name": { "family": "Singer", "given": "A." } }, { "id": "Smith-N-D", "name": { "family": "Smith", "given": "N. D." } }, { "id": "Smith-R-J-E", "name": { "family": "Smith", "given": "R. J. E." } }, { "id": "Taylor-R", "name": { "family": "Taylor", "given": "R." } }, { "id": "Thirugnanasambandam-M-P", "name": { "family": "Thirugnanasambandam", "given": "M. P." } }, { "id": "Torrie-C-I", "name": { "family": "Torrie", "given": "C. I." } }, { "id": "Vajente-G", "name": { "family": "Vajente", "given": "G." }, "orcid": "0000-0002-7656-6882" }, { "id": "Vass-S", "name": { "family": "Vass", "given": "S." } }, { "id": "Wallace-L", "name": { "family": "Wallace", "given": "L." } }, { "id": "Weinstein-Alan-J-Physics", "name": { "family": "Weinstein", "given": "A. J." }, "orcid": "0000-0002-0928-6784" }, { "id": "Williams-R-D", "name": { "family": "Williams", "given": "R. D." }, "orcid": "0000-0002-9145-8580" }, { "id": "Wipf-C-C", "name": { "family": "Wipf", "given": "C. C." } }, { "id": "Yamamoto-Hiroaki", "name": { "family": "Yamamoto", "given": "H." } }, { "id": "Zhang-Liyuan", "name": { "family": "Zhang", "given": "L." }, "orcid": "0000-0002-0898-787X" }, { "id": "Zucker-M-E", "name": { "family": "Zucker", "given": "M. E." }, "orcid": "0000-0002-2544-1596" }, { "id": "Zweizig-J", "name": { "family": "Zweizig", "given": "J." }, "orcid": "0000-0002-1521-3397" }, { "id": "Chen-Yanbei", "name": { "family": "Chen", "given": "Y." }, "orcid": "0000-0002-9730-9463" }, { "id": "Engels-W", "name": { "family": "Engels", "given": "W." } }, { "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "K. S." } }, { "id": "Hamberger-D", "name": { "family": "Hamberger", "given": "D." } }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "M. A." } }, { "id": "Szilagyi-B", "name": { "family": "Szilagyi", "given": "B." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "S." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Properties of the Binary Black Hole Merger GW150914", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2016 American Physical Society. \n\nReceived 18 February 2016; revised manuscript received 18 April 2016; published 14 June 2016. \n\nThe authors gratefully acknowledge the support of the United States National Science Foundation (NSF) for the construction and operation of the LIGO Laboratory and Advanced LIGO as well as the Science and Technology Facilities Council (STFC) of the United Kingdom, the Max-Planck-Society (MPS), and the State of Niedersachsen, Germany for support of the construction of Advanced LIGO and construction and operation of the GEO 600 detector. Additional support for Advanced LIGO was provided by the Australian Research Council. The authors gratefully acknowledge the Italian Istituto Nazionale di Fisica Nucleare (INFN), the French Centre National de la Recherche Scientifique (CNRS) and the Foundation for Fundamental Research on Matter supported by the Netherlands Organisation for Scientific Research, for the construction and operation of the Virgo detector and the creation and support of the EGO consortium. The authors also gratefully acknowledge research support from these agencies as well as by the Council of Scientific and Industrial Research of India, Department of Science and Technology, India, Science & Engineering Research Board (SERB), India, Ministry of Human Resource Development, India, the Spanish Ministerio de Econom\u00eda y Competitividad, the Conselleria d'Economia i Competitivitat and Conselleria d'Educaci\u00f3, Cultura i Universitats of the Govern de les Illes Balears, the National Science Centre of Poland, the European Commission, the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, the Hungarian Scientific Research Fund (OTKA), the Lyon Institute of Origins (LIO), the National Research Foundation of Korea, Industry Canada and the Province of Ontario through the Ministry of Economic Development and Innovation, the Natural Science and Engineering Research Council Canada, Canadian Institute for Advanced Research, the Brazilian Ministry of Science, Technology, and Innovation, Russian Foundation for Basic Research, the Leverhulme Trust, the Research Corporation, Ministry of Science and Technology (MOST), Taiwan and the Kavli Foundation. The authors gratefully acknowledge the support of the NSF, STFC, MPS, INFN, CNRS and the State of Niedersachsen, Germany for provision of computational resources.\n\nPublished - PhysRevLett.116.241102.pdf
Submitted - 1602.03840v1.pdf
", "abstract": "On September 14, 2015, the Laser Interferometer Gravitational-Wave Observatory (LIGO) detected a gravitational-wave transient (GW150914); we characterize the properties of the source and its parameters. The data around the time of the event were analyzed coherently across the LIGO network using a suite of accurate waveform models that describe gravitational waves from a compact binary system in general relativity. GW150914 was produced by a nearly equal mass binary black hole of masses 36^(+5)_(\u22124)M_\u2299 and 29^(+4)_(\u22124)M_\u2299; for each parameter we report the median value and the range of the 90% credible interval. The dimensionless spin magnitude of the more massive black hole is bound to be <0.7 (at 90% probability). The luminosity distance to the source is 410^(+160)_(\u2212180)\u2009\u2009Mpc, corresponding to a redshift 0.09+0.03\u22120.04 assuming standard cosmology. The source location is constrained to an annulus section of 610\u2009\u2009deg^2, primarily in the southern hemisphere. The binary merges into a black hole of mass 62^(+4)_(\u22124)M_\u2299 and spin 0.67^(+0.05)_(\u22120.07). This black hole is significantly more massive than any other inferred from electromagnetic observations in the stellar-mass regime.", "date": "2016-06-17", "date_type": "published", "publication": "Physical Review Letters", "volume": "116", "number": "24", "publisher": "American Physical Society", "pagerange": "Art. No. 241102", "id_number": "CaltechAUTHORS:20160616-083158343", "issn": "0031-9007", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160616-083158343", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "Max-Planck-Society" }, { "agency": "State of Niedersachsen/Germany" }, { "agency": "Australian Research Council" }, { "agency": "Istituto Nazionale di Fisica Nucleare (INFN)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)" }, { "agency": "Council of Scientific and Industrial Research (India)" }, { "agency": "Department of Science and Technology (India)" }, { "agency": "Science & Engineering Research Board (SERB)" }, { "agency": "Ministry of Human Resource Development (India)" }, { "agency": "Ministerio de Econom\u00eda y Competitividad (MINECO)" }, { "agency": "Conselleria d'Economia i Competitivitat and Conselleria d'Educaci\u00f3" }, { "agency": "Cultura i Universitats of the Govern de les Illes Balears" }, { "agency": "National Science Centre (Poland)" }, { "agency": "European Commission" }, { "agency": "Royal Society" }, { "agency": "Scottish Funding Council" }, { "agency": "Scottish Universities Physics Alliance" }, { "agency": "Hungarian Scientific Research Fund (OTKA)" }, { "agency": "Lyon Institute of Origins (LIO)" }, { "agency": "National Research Foundation of Korea" }, { "agency": "Industry Canada" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "Canadian Institute for Advanced Research (CIAR)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Inova\u00e7\u00e3o (Brazil)" }, { "agency": "Russian Foundation for Basic Research" }, { "agency": "Leverhulme Trust" }, { "agency": "Research Corporation" }, { "agency": "Ministry of Science and Technology (Taipei)" }, { "agency": "Kavli Foundation" }, { "agency": "Ontario Ministry of Economic Development and Innovation" } ] }, "local_group": { "items": [ { "id": "LIGO" } ] }, "corp_creators": { "items": [ "LIGO Scientific Collaboration", "Virgo Collaboration" ] }, "doi": "10.1103/PhysRevLett.116.241102", "primary_object": { "basename": "1602.03840v1.pdf", "url": "https://authors.library.caltech.edu/records/mt5ym-r8015/files/1602.03840v1.pdf" }, "related_objects": [ { "basename": "PhysRevLett.116.241102.pdf", "url": "https://authors.library.caltech.edu/records/mt5ym-r8015/files/PhysRevLett.116.241102.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Abbott, B. P.; Abbott, R.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/qqfw7-0x416", "eprint_id": 67944, "eprint_status": "archive", "datestamp": "2023-09-15 05:27:11", "lastmod": "2023-10-23 21:17:35", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Abbott-B-P", "name": { "family": "Abbott", "given": "B. P." } }, { "id": "Abbott-R", "name": { "family": "Abbott", "given": "R." } }, { "id": "Adhikari-R-X", "name": { "family": "Adhikari", "given": "R. X." }, "orcid": "0000-0002-5731-5076" }, { "id": "Anderson-S-B", "name": { "family": "Anderson", "given": "S. B." } }, { "id": "Arai-Koji", "name": { "family": "Arai", "given": "K." }, "orcid": "0000-0001-8916-8915" }, { "id": "Araya-M-C", "name": { "family": "Araya", "given": "M. C." } }, { "id": "Barayoga-J-C", "name": { "family": "Barayoga", "given": "J. C." } }, { "id": "Barish-B-C", "name": { "family": "Barish", "given": "B. 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D." }, "orcid": "0000-0002-9145-8580" }, { "id": "Wipf-C-C", "name": { "family": "Wipf", "given": "C. C." } }, { "id": "Yamamoto-Hiroaki", "name": { "family": "Yamamoto", "given": "H." } }, { "id": "Zhang-Liyuan", "name": { "family": "Zhang", "given": "L." }, "orcid": "0000-0002-0898-787X" }, { "id": "Zucker-M-E", "name": { "family": "Zucker", "given": "M. E." }, "orcid": "0000-0002-2544-1596" }, { "id": "Zweizig-J", "name": { "family": "Zweizig", "given": "J." }, "orcid": "0000-0002-1521-3397" }, { "id": "Chen-Yanbei", "name": { "family": "Chen", "given": "Y." }, "orcid": "0000-0002-9730-9463" }, { "id": "Engels-W", "name": { "family": "Engels", "given": "W." } }, { "id": "Schmidt-P", "name": { "family": "Schmidt", "given": "P." } }, { "id": "Vallisneri-M", "name": { "family": "Vallisneri", "given": "M." }, "orcid": "0000-0002-4162-0033" }, { "id": "Hemberger-D-A", "name": { "family": "Hemberger", "given": "D." } }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "M." } }, { "id": "Szil\u00e1gyi-B", "name": { "family": "Szil\u00e1gyi", "given": "B." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "S." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "GW151226: Observation of Gravitational Waves from a 22-Solar-Mass Binary Black Hole Coalescence", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2015 Published by the American Physical Society.This article is available under the terms of the Creative Commons Attribution 3.0 License. Further distribution of this work must maintain attribution to the author(s) and the published article's title, journal citation, and DOI. \n\nReceived 31 May 2016; published 15 June 2016. \n\nThe authors gratefully acknowledge the support of the United States National Science Foundation (NSF) for the construction and operation of the LIGO Laboratory and Advanced LIGO as well as the Science and Technology Facilities Council (STFC) of the United Kingdom, the Max Planck Society (MPS), and the State of Niedersachsen/Germany for support of the construction of Advanced LIGO and construction and operation of the GEO600 detector. Additional support for Advanced LIGO was provided by the Australian Research Council. The authors gratefully acknowledge the Italian Istituto Nazionale di Fisica Nucleare (INFN), the French Centre National de la Recherche Scientifique (CNRS) and the Foundation for Fundamental Research on Matter supported by the Netherlands Organisation for Scientific Research, for the construction and operation of the Virgo detector and the creation and support of the EGO consortium. The authors also gratefully acknowledge research support from these agencies as well as by the Council of Scientific and Industrial Research of India, Department of Science and Technology, India, Science & Engineering Research Board (SERB), India, Ministry of Human Resource Development, India, the Spanish Ministerio de Econom\u00eda y Competitividad, the Conselleria d'Economia i Competitivitat and Conselleria d'Educaci\u00f3, Cultura i Universitats of the Govern de les Illes Balears, the National Science Centre of Poland, the European Commission, the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, the Hungarian Scientific Research Fund (OTKA), the Lyon Institute of Origins (LIO), the National Research Foundation of Korea, Industry Canada and the Province of Ontario through the Ministry of Economic Development and Innovation, the Natural Sciences and Engineering Research Council of Canada, Canadian Institute for Advanced Research, the Brazilian Ministry of Science, Technology, and Innovation, Funda\u00e7\u00e3o de Amparo \u00e0 Pesquisa do Estado de S\u00e3o Paulo (FAPESP), Russian Foundation for Basic Research, the Leverhulme Trust, the Research Corporation, Ministry of Science and Technology (MOST), Taiwan, and the Kavli Foundation. The authors gratefully acknowledge the support of the NSF, STFC, MPS, INFN, CNRS and the State of Niedersachsen/Germany for provision of computational resources. \n\nThis article has been assigned the document numbers LIGO-P151226 and VIR-0285A-16.\n\nPublished - PhysRevLett.116.241103.pdf
", "abstract": "We report the observation of a gravitational-wave signal produced by the coalescence of two stellar-mass black holes. The signal, GW151226, was observed by the twin detectors of the Laser Interferometer Gravitational-Wave Observatory (LIGO) on December 26, 2015 at 03:38:53 UTC. The signal was initially identified within 70 s by an online matched-filter search targeting binary coalescences. Subsequent off-line analyses recovered GW151226 with a network signal-to-noise ratio of 13 and a significance greater than 5\u03c3. The signal persisted in the LIGO frequency band for approximately 1 s, increasing in frequency and amplitude over about 55 cycles from 35 to 450 Hz, and reached a peak gravitational strain of 3.4^(+0.7)_(-0.9) \u00d710^(-22). The inferred source-frame initial black hole masses are 14.2^(+8.3)_(-3.7) M\u2299 and 7.5^(+2.3)_(-2.3) M\u2299, and the final black hole mass is 20.8^(+6.1)_(-1.7) M\u2299. We find that at least one of the component black holes has spin greater than 0.2. This source is located at a luminosity distance of 440^(+180)_(-190)\u2009Mpc corresponding to a redshift of 0.09^(+0.03)_(-0.04). All uncertainties define a 90% credible interval. This second gravitational-wave observation provides improved constraints on stellar populations and on deviations from general relativity.", "date": "2016-06-15", "date_type": "published", "publication": "Physical Review Letters", "volume": "116", "number": "24", "publisher": "American Physical Society", "pagerange": "Art. No. 241103", "id_number": "CaltechAUTHORS:20160615-122950563", "issn": "0031-9007", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160615-122950563", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "Max Planck Society" }, { "agency": "State of Niedersachsen/Germany" }, { "agency": "Australian Research Council" }, { "agency": "Istituto Nazionale di Fisica Nucleare (INFN)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)" }, { "agency": "Council of Scientific and Industrial Research (India)" }, { "agency": "Department of Science and Technology (India)" }, { "agency": "Science & Engineering Research Board (SERB)" }, { "agency": "Ministry of Human Resource Development (India)" }, { "agency": "Ministerio de Econom\u00eda y Competitividad (MINECO)" }, { "agency": "Conselleria d'Economia i Competitivitat" }, { "agency": "Conselleria d'Educaci\u00f3, Cultura i Universitats of the Govern de les Illes Balears" }, { "agency": "National Science Centre of Poland" }, { "agency": "European Commission" }, { "agency": "Royal Society" }, { "agency": "Scottish Funding Council" }, { "agency": "Scottish Universities Physics Alliance" }, { "agency": "Hungarian Scientific Research Fund (OTKA)" }, { "agency": "Lyon Institute of Origins (LIO)" }, { "agency": "National Research Foundation of Korea" }, { "agency": "Industry Canada" }, { "agency": "Ontario Ministry of Economic Development and Innovation" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "Canadian Institute for Advanced Research (CIAR)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Inova\u00e7\u00e3o (MCTI)" }, { "agency": "Funda\u00e7\u00e3o de Amparo \u00e0 Pesquisa do Estado de S\u00e3o Paulo (FAPESP)" }, { "agency": "Russian Foundation for Basic Research" }, { "agency": "Leverhulme Trust" }, { "agency": "Research Corporation" }, { "agency": "Ministry of Science and Technology (Taipei)" }, { "agency": "Kavli Foundation" } ] }, "other_numbering_system": { "items": [ { "id": "VIR-0285A-16", "name": "VIRGO Document" } ] }, "local_group": { "items": [ { "id": "LIGO" } ] }, "corp_creators": { "items": [ "LIGO Scientific Collaboration", "Virgo Collaboration" ] }, "doi": "10.1103/PhysRevLett.116.241103", "primary_object": { "basename": "PhysRevLett.116.241103.pdf", "url": "https://authors.library.caltech.edu/records/qqfw7-0x416/files/PhysRevLett.116.241103.pdf" }, "resource_type": "article", "pub_year": "2016", "author_list": "Abbott, B. P.; Abbott, R.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/mr2zm-tzn07", "eprint_id": 67757, "eprint_status": "archive", "datestamp": "2023-08-20 12:04:20", "lastmod": "2023-10-18 21:40:33", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Abbott-B-P", "name": { "family": "Abbott", "given": "B. P." } }, { "id": "Abbott-R", "name": { "family": "Abbott", "given": "R." } }, { "id": "Abernathy-M-R", "name": { "family": "Abernathy", "given": "M. R." } }, { "id": "Adhikari-R-X", "name": { "family": "Adhikari", "given": "R. X." }, "orcid": "0000-0002-5731-5076" }, { "id": "Anderson-S-B", "name": { "family": "Anderson", "given": "S. B." } }, { "id": "Arai-Koji", "name": { "family": "Arai", "given": "K." }, "orcid": "0000-0001-8916-8915" }, { "id": "Araya-M-C", "name": { "family": "Araya", "given": "M. C." } }, { "id": "Barayoga-J-C", "name": { "family": "Barayoga", "given": "J. C." } }, { "id": "Barish-B-C", "name": { "family": "Barish", "given": "B. C." } }, { "id": "Berger-B-K", "name": { "family": "Berger", "given": "B. K." } }, { "id": "Billingsley-G", "name": { "family": "Billingsley", "given": "G." }, "orcid": "0000-0002-4141-2744" }, { "id": "Blackburn-J-K", "name": { "family": "Blackburn", "given": "J. K." }, "orcid": "0000-0002-3838-2986" }, { "id": "Bork-R", "name": { "family": "Bork", "given": "R." } }, { "id": "Brooks-A-F", "name": { "family": "Brooks", "given": "A. F." }, "orcid": "0000-0003-4295-792X" }, { "id": "Cahillane-C", "name": { "family": "Cahillane", "given": "C." } }, { "id": "Callister-T-A", "name": { "family": "Callister", "given": "T." }, "orcid": "0000-0001-9892-177X" }, { "id": "Cepeda-C-B", "name": { "family": "Cepeda", "given": "C. B." } }, { "id": "Chakraborty-R", "name": { "family": "Chakraborty", "given": "R." } }, { "id": "Chalermsongsak-T", "name": { "family": "Chalermsongsak", "given": "T." } }, { "id": "Couvares-P", "name": { "family": "Couvares", "given": "P." } }, { "id": "Coyne-D-C", "name": { "family": "Coyne", "given": "D. C." }, "orcid": "0000-0002-6427-3222" }, { "id": "Dergachev-V", "name": { "family": "Dergachev", "given": "V." } }, { "id": "Drever-R-W-P", "name": { "family": "Drever", "given": "R. W. P." } }, { "id": "Ehrens-P", "name": { "family": "Ehrens", "given": "P." } }, { "id": "Etzel-T", "name": { "family": "Etzel", "given": "T." } }, { "id": "Gossan-S-E", "name": { "family": "Gossan", "given": "S. E." }, "orcid": "0000-0002-8138-9198" }, { "id": "Gushwa-K-E", "name": { "family": "Gushwa", "given": "K. E." } }, { "id": "Gustafson-E-K", "name": { "family": "Gustafson", "given": "E. K." } }, { "id": "Hall-E-D", "name": { "family": "Hall", "given": "E. D." }, "orcid": "0000-0001-9018-666X" }, { "id": "Heptonstall-A-W", "name": { "family": "Heptonstall", "given": "A. W." } }, { "id": "Hodge-K-A", "name": { "family": "Hodge", "given": "K. A." } }, { "id": "Isi-M", "name": { "family": "Isi", "given": "M." }, "orcid": "0000-0001-8830-8672" }, { "id": "Kanner-J-B", "name": { "family": "Kanner", "given": "J. B." }, "orcid": "0000-0001-8115-0577" }, { "id": "Kells-W", "name": { "family": "Kells", "given": "W." } }, { "id": "Kondrashov-V", "name": { "family": "Kondrashov", "given": "V." } }, { "id": "Korth-W-Z", "name": { "family": "Korth", "given": "W. Z." }, "orcid": "0000-0003-3527-1348" }, { "id": "Kozak-D-B", "name": { "family": "Kozak", "given": "D. B." }, "orcid": "0000-0003-3118-8950" }, { "id": "Lazzarini-A", "name": { "family": "Lazzarini", "given": "A." } }, { "id": "Li-T-G-F", "name": { "family": "Li", "given": "T. G. F." } }, { "id": "Mageswaran-M", "name": { "family": "Mageswaran", "given": "M." } }, { "id": "Maros-E", "name": { "family": "Maros", "given": "E." } }, { "id": "Martynov-D-V", "name": { "family": "Martynov", "given": "D. V." } }, { "id": "Marx-J-N", "name": { "family": "Marx", "given": "J. N." } }, { "id": "McIntyre-G", "name": { "family": "McIntyre", "given": "G." } }, { "id": "McIver-J", "name": { "family": "McIver", "given": "J." }, "orcid": "0000-0003-0316-1355" }, { "id": "Meshkov-S", "name": { "family": "Meshkov", "given": "S." } }, { "id": "Pedraza-M", "name": { "family": "Pedraza", "given": "M." } }, { "id": "Perreca-A", "name": { "family": "Perreca", "given": "A." } }, { "id": "Price-L-R", "name": { "family": "Price", "given": "L. R." } }, { "id": "Quintero-E-A", "name": { "family": "Quintero", "given": "E. A." } }, { "id": "Robertson-N-A", "name": { "family": "Robertson", "given": "N. A." } }, { "id": "Rollins-J-G", "name": { "family": "Rollins", "given": "J. G." } }, { "id": "Sachdev-S", "name": { "family": "Sachdev", "given": "S." }, "orcid": "0000-0002-2432-7070" }, { "id": "Sanchez-E-J", "name": { "family": "Sanchez", "given": "E. J." } }, { "id": "Schmidt-P", "name": { "family": "Schmidt", "given": "P." } }, { "id": "Shao-Z", "name": { "family": "Shao", "given": "Z." } }, { "id": "Singer-A", "name": { "family": "Singer", "given": "A." } }, { "id": "Smith-N-D", "name": { "family": "Smith", "given": "N. D." } }, { "id": "Smith-R-J-E", "name": { "family": "Smith", "given": "R. J. E." } }, { "id": "Taylor-R", "name": { "family": "Taylor", "given": "R." } }, { "id": "Thirugnanasambandam-M-P", "name": { "family": "Thirugnanasambandam", "given": "M. P." } }, { "id": "Torrie-C-I", "name": { "family": "Torrie", "given": "C. I." } }, { "id": "Vajente-G", "name": { "family": "Vajente", "given": "G." }, "orcid": "0000-0002-7656-6882" }, { "id": "Vass-S", "name": { "family": "Vass", "given": "S." } }, { "id": "Wallace-L", "name": { "family": "Wallace", "given": "L." } }, { "id": "Weinstein-Alan-J-Physics", "name": { "family": "Weinstein", "given": "A. J." }, "orcid": "0000-0002-0928-6784" }, { "id": "Williams-R-D", "name": { "family": "Williams", "given": "R. D." }, "orcid": "0000-0002-9145-8580" }, { "id": "Wipf-C-C", "name": { "family": "Wipf", "given": "C. C." } }, { "id": "Yamamoto-Hiroaki", "name": { "family": "Yamamoto", "given": "H." } }, { "id": "Zhang-Liyuan", "name": { "family": "Zhang", "given": "L." }, "orcid": "0000-0002-0898-787X" }, { "id": "Zucker-M-E", "name": { "family": "Zucker", "given": "M. E." }, "orcid": "0000-0002-2544-1596" }, { "id": "Zweizig-J", "name": { "family": "Zweizig", "given": "J." }, "orcid": "0000-0002-1521-3397" }, { "id": "Chen-Yanbei", "name": { "family": "Chen", "given": "Y." }, "orcid": "0000-0002-9730-9463" }, { "id": "Engels-W", "name": { "family": "Engels", "given": "W." } }, { "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "K. S." } }, { "id": "Vallisneri-M", "name": { "family": "Vallisneri", "given": "M." }, "orcid": "0000-0002-4162-0033" }, { "id": "Hemberger-D-A", "name": { "family": "Hemberger", "given": "D. A." } }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "M. A." } }, { "id": "Szilagyi-B", "name": { "family": "Szilagyi", "given": "B." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "S." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Tests of General Relativity with GW150914", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2016 American Physical Society. \n\nReceived 26 March 2016; revised manuscript received 9 May 2016; published 31 May 2016. \n\nThe authors gratefully acknowledge the support of the U.S. National Science Foundation (NSF) for the construction and operation of the LIGO Laboratory and Advanced LIGO as well as the Science and Technology Facilities Council (STFC) of the United Kingdom, the Max-Planck-Society (MPS), and the State of Niedersachsen/Germany for support of the construction of Advanced LIGO and construction and operation of the GEO600 detector. Additional support for Advanced LIGO was provided by the Australian Research Council. The authors gratefully acknowledge the Italian Istituto Nazionale di Fisica Nucleare (INFN), the French Centre National de la Recherche Scientifique (CNRS), and the Foundation for Fundamental Research on Matter supported by the Netherlands Organisation for Scientific Research, for the construction and operation of the Virgo detector and the creation and support of the EGO consortium. The authors also gratefully acknowledge research support from these agencies as well as by the Council of Scientific and Industrial Research of India, Department of Science and Technology, India, Science and Engineering Research Board (SERB), India, Ministry of Human Resource Development, India, the Spanish Ministerio de Econom\u00eda y Competitividad, the Conselleria d'Economia i Competitivitat and Conselleria d'Educaci\u00f3, Cultura i Universitats of the Govern de les Illes Balears, the National Science Centre of Poland, the European Commission, the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, the Hungarian Scientific Research Fund (OTKA), the Lyon Institute of Origins (LIO), the National Research Foundation of Korea, Industry Canada and the Province of Ontario through the Ministry of Economic Development and Innovation, the Natural Science and Engineering Research Council Canada, the Canadian Institute for Advanced Research, the Brazilian Ministry of Science, Technology, and Innovation, the Russian Foundation for Basic Research, the Leverhulme Trust, the Research Corporation, Ministry of Science and Technology (MOST), Taiwan, and the Kavli Foundation. The authors gratefully acknowledge the support of the NSF, STFC, MPS, INFN, CNRS, and the State of Niedersachsen/Germany for the provision of computational resources. \n\nFinally, we thank the anonymous referees, whose comments helped improve the clarity of the Letter.\n\nPublished - PhysRevLett.116.221101.pdf
Submitted - 1602.03841v2.pdf
", "abstract": "The LIGO detection of GW150914 provides an unprecedented opportunity to study the two-body motion of a compact-object binary in the large-velocity, highly nonlinear regime, and to witness the final merger of the binary and the excitation of uniquely relativistic modes of the gravitational field. We carry out several investigations to determine whether GW150914 is consistent with a binary black-hole merger in general relativity. We find that the final remnant's mass and spin, as determined from the low-frequency (inspiral) and high-frequency (postinspiral) phases of the signal, are mutually consistent with the binary black-hole solution in general relativity. Furthermore, the data following the peak of GW150914 are consistent with the least-damped quasinormal mode inferred from the mass and spin of the remnant black hole. By using waveform models that allow for parametrized general-relativity violations during the inspiral and merger phases, we perform quantitative tests on the gravitational-wave phase in the dynamical regime and we determine the first empirical bounds on several high-order post-Newtonian coefficients. We constrain the graviton Compton wavelength, assuming that gravitons are dispersed in vacuum in the same way as particles with mass, obtaining a 90%-confidence lower bound of 10^(13\u2009)\u2009km. In conclusion, within our statistical uncertainties, we find no evidence for violations of general relativity in the genuinely strong-field regime of gravity.", "date": "2016-06-03", "date_type": "published", "publication": "Physical Review Letters", "volume": "116", "number": "22", "publisher": "American Physical Society", "pagerange": "Art. No. 221101", "id_number": "CaltechAUTHORS:20160607-154130083", "issn": "0031-9007", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160607-154130083", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "Max-Planck-Society" }, { "agency": "State of Niedersachsen/Germany" }, { "agency": "Australian Research Council" }, { "agency": "Istituto Nazionale di Fisica Nucleare (INFN)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Stichting voor Fundamenteel Onderzoek der Materie (FOM)" }, { "agency": "Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)" }, { "agency": "Council of Scientific and Industrial Research (India)" }, { "agency": "Department of Science and Technology (India)" }, { "agency": "Science and Engineering Research Board (SERB)" }, { "agency": "Ministry of Human Resource Development (India)" }, { "agency": "Ministerio de Econom\u00eda y Competitividad (MINECO)" }, { "agency": "Conselleria d'Economia i Competitivitat and Conselleria d'Educaci\u00f3" }, { "agency": "Cultura i Universitats of the Govern de les Illes Balears" }, { "agency": "National Science Centre of Poland" }, { "agency": "European Commission" }, { "agency": "Royal Society" }, { "agency": "Scottish Funding Council" }, { "agency": "Scottish Universities Physics Alliance" }, { "agency": "Hungarian Scientific Research Fund (OTKA)" }, { "agency": "Lyon Institute of Origins (LIO)" }, { "agency": "National Research Foundation of Korea" }, { "agency": "Industry Canada" }, { "agency": "Natural Science and Engineering Research Council of Canada (NSERC)" }, { "agency": "Canadian Institute for Advanced Research (CIAR)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Inova\u00e7\u00e3o (MCTI)" }, { "agency": "Russian Foundation for Basic Research" }, { "agency": "Leverhulme Trust" }, { "agency": "Research Corporation" }, { "agency": "Ministry of Science and Technology (Taipei)" }, { "agency": "Kavli Foundation" }, { "agency": "Ontario Ministry of Research and Innovation" } ] }, "local_group": { "items": [ { "id": "LIGO" } ] }, "corp_creators": { "items": [ "LIGO Scientific Collaboration", "Virgo Collaboration" ] }, "doi": "10.1103/PhysRevLett.116.221101", "primary_object": { "basename": "1602.03841v2.pdf", "url": "https://authors.library.caltech.edu/records/mr2zm-tzn07/files/1602.03841v2.pdf" }, "related_objects": [ { "basename": "PhysRevLett.116.221101.pdf", "url": "https://authors.library.caltech.edu/records/mr2zm-tzn07/files/PhysRevLett.116.221101.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Abbott, B. P.; Abbott, R.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/6wa27-mg134", "eprint_id": 86815, "eprint_status": "archive", "datestamp": "2023-08-20 11:41:21", "lastmod": "2023-10-18 20:36:40", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Henriksson-K", "name": { "family": "Henriksson", "given": "Katherine" } }, { "id": "Foucart-F", "name": { "family": "Foucart", "given": "Fran\u00e7ois" }, "orcid": "0000-0003-4617-4738" }, { "id": "Kidder-L-E", "name": { "family": "Kidder", "given": "Lawrence E." }, "orcid": "0000-0001-5392-7342" }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Initial data for high-compactness black hole\u2013neutron star binaries", "ispublished": "pub", "full_text_status": "public", "keywords": "neutron stars, initial value problem, black holes, relativity and gravitation, relativistic binaries", "note": "\u00a9 2016 IOP Publishing Ltd. \n\nReceived 22 January 2016. Accepted for publication 26 February 2016. Published 19 April 2016. \n\nK H would like to thank Geoffrey Lovelace, Curran Muhlberger, Harald Pfeiffer, and David Chernoff for useful discussions, and Andy Bohn for the use of computing resources. This work was supported in part by NSF Grants PHY-1306125 and AST-1333129 at Cornell University, and by a grant from the Sherman Fairchild Foundation. F F gratefully acknowledges support from the Vincent and Beatrice Tremaine Postdoctoral Fellowship and NSERC Canada. Support for this work was provided by NASA through Einstein Postdoctoral Fellowship grant number PF4-150122 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. This research was performed in part using the Zwicky computer system operated by the Caltech Center for Advanced Computing Research and funded by NSF MRI No. PHY-0960291 and the Sherman Fairchild Foundation.\n\nSubmitted - 1409.7159
", "abstract": "For highly compact neutron stars, constructing numerical initial data for black hole\u2013neutron star binary evolutions is very difficult. We describe improvements to an earlier method that enable it to handle these more challenging cases. These improvements were found by invoking a general relaxation principle that may be helpful in improving robustness in other initial data solvers. We examine the case of a 6:1 mass ratio system in inspiral close to merger, where the star is governed by a polytropic \u0393 =2, an SLy, or an LS220 equation of state (EOS). In particular, we are able to obtain a solution with a realistic LS220 EOS for a star with compactness 0.26 and mass 1.98 M_\u2299, which is representative of the highest reliably determined neutron star masses. For the SLy EOS, we can obtain solutions with a comparable compactness of 0.25, while for a family of polytropic equations of state, we obtain solutions with compactness up to 0.21, the largest compactness that is stable in this family. These compactness values are significantly higher than any previously published results.", "date": "2016-05-19", "date_type": "published", "publication": "Classical and Quantum Gravity", "volume": "33", "number": "10", "publisher": "IOP", "pagerange": "Art. no. 105009", "id_number": "CaltechAUTHORS:20180605-163331410", "issn": "0264-9381", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180605-163331410", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY-1306125" }, { "agency": "NSF", "grant_number": "AST-1333129" }, { "agency": "Sherman Fairchild Foundation" }, { "agency": "Vincent and Beatrice Tremaine Postdoctoral Fellowship" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "NASA Einstein Fellowship", "grant_number": "PF4-150122" }, { "agency": "NASA", "grant_number": "NAS8-03060" }, { "agency": "NSF", "grant_number": "PHY-0960291" } ] }, "doi": "10.1088/0264-9381/33/10/105009", "primary_object": { "basename": "1409.7159", "url": "https://authors.library.caltech.edu/records/6wa27-mg134/files/1409.7159" }, "resource_type": "article", "pub_year": "2016", "author_list": "Henriksson, Katherine; Foucart, Fran\u00e7ois; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/0cx2m-cct58", "eprint_id": 66012, "eprint_status": "archive", "datestamp": "2023-08-22 17:56:23", "lastmod": "2023-10-18 17:03:29", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Formulation of discontinuous Galerkin methods for relativistic astrophysics", "ispublished": "pub", "full_text_status": "public", "keywords": "Discontinuous Galerkin; Hydrodynamics; Magnetohydrodynamics; Einstein's equations; Moving mesh; Arbitrary Lagrangian\u2013Eulerian (ALE); Metric identities; Geometric conservation law", "note": "\u00a9 2016 Elsevier Inc.\n\nReceived 27 July 2015; Received in revised form 10 December 2015; Accepted 11 February 2016; Available online 17 February 2016.\n\nI thank Fran\u00e7ois H\u00e9bert for helpful discussions. I am grateful for the hospitality of TAPIR and the Walter Burke Institute for Theoretical Physics at Caltech where part of this work was carried out. This work was supported in part by NSF Grants PHY-1306125 and AST-1333129 at Cornell University, and by a grant from the Sherman Fairchild Foundation.\n\nSubmitted - 1510.pdf
", "abstract": "The DG algorithm is a powerful method for solving pdes, especially for evolution equations in conservation form. Since the algorithm involves integration over volume elements, it is not immediately obvious that it will generalize easily to arbitrary time-dependent curved spacetimes. We show how to formulate the algorithm in such spacetimes for applications in relativistic astrophysics. We also show how to formulate the algorithm for equations in non-conservative form, such as Einstein's field equations themselves. We find two computationally distinct formulations in both cases, one of which has seldom been used before for flat space in curvilinear coordinates but which may be more efficient. We also give a new derivation of the ALE algorithm (Arbitrary Lagrangian\u2013Eulerian) using 4-vector methods that is much simpler than the usual derivation and explains why the method preserves the conservation form of the equations. The various formulations are explored with some simple numerical experiments that also investigate the effect of the metric identities on the results. The results of this paper may also be of interest to practitioners of DG working with curvilinear elements in flat space.", "date": "2016-05-01", "date_type": "published", "publication": "Journal of Computational Physics", "volume": "312", "publisher": "Elsevier", "pagerange": "333-356", "id_number": "CaltechAUTHORS:20160408-083733301", "issn": "0021-9991", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160408-083733301", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY-1306125" }, { "agency": "NSF", "grant_number": "AST-1333129" }, { "agency": "Sherman Fairchild Foundation" } ] }, "local_group": { "items": [ { "id": "TAPIR" }, { "id": "Walter-Burke-Institute-for-Theoretical-Physics" } ] }, "doi": "10.1016/j.jcp.2016.02.031", "primary_object": { "basename": "1510.pdf", "url": "https://authors.library.caltech.edu/records/0cx2m-cct58/files/1510.pdf" }, "resource_type": "article", "pub_year": "2016", "author_list": "Teukolsky, Saul A." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/ga3na-ap255", "eprint_id": 86816, "eprint_status": "archive", "datestamp": "2023-08-20 07:01:39", "lastmod": "2023-10-18 20:36:45", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "The Kerr metric", "ispublished": "pub", "full_text_status": "public", "keywords": "Kerr metric, black holes, Kerr perturbations", "note": "\u00a9 2015 IOP Publishing Ltd. \n\nReceived 10 September 2014. Accepted for publication 8 October 2014. Published 1 June 2015. \n\nFocus issue: Milestones of general relativity \n\nI thank Leo Stein, Stanley Deser and Ted Jacobson for helpful discussions. This work was supported in part by NSF Grants PHY-1306125 and AST-1333129 at Cornell University, and by a grant from the Sherman Fairchild Foundation.\n\nSubmitted - 1410.2130.pdf
", "abstract": "This review describes the events leading up to the discovery of the Kerr metric in 1963 and the enormous impact the discovery has had in the subsequent 50 years. The review discusses the Penrose process, the four laws of black hole mechanics, uniqueness of the solution, and the no-hair theorems. It also includes Kerr perturbation theory and its application to black hole stability and quasi-normal modes. The Kerr metric's importance in the astrophysics of quasars and accreting stellar-mass black hole systems is detailed. A theme of the review is the 'miraculous' nature of the solution, both in describing in a simple analytic formula the most general rotating black hole, and in having unexpected mathematical properties that make many calculations tractable. Also included is a pedagogical derivation of the solution suitable for a first course in general relativity.", "date": "2015-06-25", "date_type": "published", "publication": "Classical and Quantum Gravity", "volume": "32", "number": "12", "publisher": "IOP", "pagerange": "Art. No. 124006", "id_number": "CaltechAUTHORS:20180605-164020178", "issn": "0264-9381", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180605-164020178", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY-1306125" }, { "agency": "NSF", "grant_number": "AST-1333129" }, { "agency": "Sherman Fairchild Foundation" } ] }, "doi": "10.1088/0264-9381/32/12/124006", "primary_object": { "basename": "1410.2130.pdf", "url": "https://authors.library.caltech.edu/records/ga3na-ap255/files/1410.2130.pdf" }, "resource_type": "article", "pub_year": "2015", "author_list": "Teukolsky, Saul A." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/snjps-h7263", "eprint_id": 86801, "eprint_status": "archive", "datestamp": "2023-08-22 14:58:00", "lastmod": "2023-10-18 20:36:01", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Short note on the mass matrix for Gauss\u2013Lobatto grid points", "ispublished": "pub", "full_text_status": "public", "keywords": "Mass matrix; Gauss\u2013Lobatto quadrature; Spectral methods; Discontinuous Galerkin methods; Finite element methods", "note": "\u00a9 2014 Elsevier Inc. \n\nReceived 16 September 2014, Revised 20 November 2014, Accepted 6 December 2014, Available online 12 December 2014. \n\nI thank Jan Hesthaven for several helpful comments, including pointing out that interpolation from a coarse grid to a finer one introduces no aliasing. This work was supported in part by NSF Grants PHY-1306125 and AST-1333129 at Cornell University, and by a grant from the Sherman Fairchild Foundation.\n\nSubmitted - 1412.2276.pdf
", "abstract": "The mass matrix for Gauss\u2013Lobatto grid points is usually approximated by Gauss\u2013Lobatto quadrature because this leads to a diagonal matrix that is easy to invert. The exact mass matrix and its inverse are full. We show that the exact mass matrix and its inverse differ from the approximate diagonal ones by a simple rank-1 update (outer product). They can thus be applied to an arbitrary vector in O(N) operations instead of O(N^2).", "date": "2015-02-15", "date_type": "published", "publication": "Journal of Computational Physics", "volume": "283", "publisher": "Elsevier", "pagerange": "408-413", "id_number": "CaltechAUTHORS:20180605-142355801", "issn": "0021-9991", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180605-142355801", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY-1306125" }, { "agency": "NSF", "grant_number": "AST-1333129" }, { "agency": "Sherman Fairchild Foundation" } ] }, "doi": "10.1016/j.jcp.2014.12.012", "primary_object": { "basename": "1412.2276.pdf", "url": "https://authors.library.caltech.edu/records/snjps-h7263/files/1412.2276.pdf" }, "resource_type": "article", "pub_year": "2015", "author_list": "Teukolsky, Saul A." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/dd3xx-a2d03", "eprint_id": 53255, "eprint_status": "archive", "datestamp": "2023-08-20 03:42:13", "lastmod": "2023-10-19 14:41:38", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Muhlberger-C-D", "name": { "family": "Muhlberger", "given": "Curran D." } }, { "id": "Nouri-F-H", "name": { "family": "Nouri", "given": "Fatemeh Hossein" } }, { "id": "Duez-M-D", "name": { "family": "Duez", "given": "Matthew D." }, "orcid": "0000-0002-0050-1783" }, { "id": "Foucart-F", "name": { "family": "Foucart", "given": "Francois" }, "orcid": "0000-0003-4617-4738" }, { "id": "Kidder-L-E", "name": { "family": "Kidder", "given": "Lawrence E." }, "orcid": "0000-0001-5392-7342" }, { "id": "Ott-C-D", "name": { "family": "Ott", "given": "Christian D." }, "orcid": "0000-0003-4993-2055" }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." } }, { "id": "Szil\u00e1gyi-B", "name": { "family": "Szil\u00e1gyi", "given": "B\u00e9la" } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Magnetic effects on the low-T/|W| instability in differentially rotating neutron stars", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2014 American Physical Society.\n\nReceived 12 May 2014; published 17 November 2014.\n\nWe extend our thanks to D. Lai for inspiring this\ninvestigation, to M. Boyle for advice on several occasions,\nand to F. H\u00e9bert for catching errors in the text. We also\nextend our gratitude to S. Bernuzzi, R. De Pietri, B.\nGiacomazzo, and L. Rezzolla, whose correspondence\nafter the first version of this paper helped to clarify the\ncomparison between their simulations and ours. The\nauthors at Cornell gratefully acknowledge support from\nNational Science Foundation (NSF) Grants No. PHY-\n1306125 and No. AST-1333129, while the authors at\nCaltech acknowledge support from NSF Grants\nNo. PHY-1440083 and No. AST-1333520 and NSF\nCAREER Award No. PHY-1151197. Authors at both\nCaltech and Cornell also thank the Sherman Fairchild\nFoundation for their support. F. Foucart gratefully acknowledges\nsupport from the Vincent and Beatrice Tremaine\nPostdoctoral Fellowship, from the NSERC of Canada, from\nthe Canada Research Chairs Program, and from the\nCanadian Institute for Theoretical Astrophysics. Finally,\nthe authors at WSU acknowledge support through NASA\nGrant No. NNX11AC37G and NSF Grant No. PHY-1402916. Some computations were performed on the\nGPC supercomputer at the SciNet HPC Consortium\n[53], funded by the Canada Foundation for Innovation\nunder the auspices of Compute Canada, the Government\nof Ontario, Ontario Research Fund\u2013Research Excellence,\nand the University of Toronto. This work also used the\nExtreme Science and Engineering Discovery Environment\n(XSEDE) through allocations No. TG-PHY100033 and\nNo. PHY990002, supported by NSF Grant No. OCI-1053575. Additionally, this research was performed in part\nusing the Zwicky computer system operated by the Caltech\nCenter for Advanced Computing Research and funded by\nNSF MRI No. PHY-0960291 and the Sherman Fairchild\nFoundation.\n\nPublished - PhysRevD.90.104014.pdf
Submitted - 1405.2144v1.pdf
", "abstract": "Dynamical instabilities in protoneutron stars may produce gravitational waves whose observation could shed light on the physics of core-collapse supernovae. When born with sufficient differential rotation, these stars are susceptible to a shear instability (the \"low-T/|W| instability\"), but such rotation can also amplify magnetic fields to strengths where they have a considerable impact on the dynamics of the stellar matter. Using a new magnetohydrodynamics module for the Spectral Einstein Code, we have simulated a differentially-rotating neutron star in full 3D to study the effects of magnetic fields on this instability. Though strong toroidal fields were predicted to suppress the low-T/|W| instability, we find that they do so only in a small range of field strengths. Below 4\u00d710^(13) G, poloidal seed fields do not wind up fast enough to have an effect before the instability saturates, while above 5\u00d710^(14) G, magnetic instabilities can actually amplify a global quadrupole mode (this threshold may be even lower in reality, as small-scale magnetic instabilities remain difficult to resolve numerically). Thus, the prospects for observing gravitational waves from such systems are not in fact diminished over most of the magnetic parameter space. Additionally, we report that the detailed development of the low-T/|W| instability, including its growth rate, depends strongly on the particular numerical methods used. The high-order methods we employ suggest that growth might be considerably slower than found in some previous simulations.", "date": "2014-11-15", "date_type": "published", "publication": "Physical Review D", "volume": "90", "number": "10", "publisher": "American Physical Society", "pagerange": "Art. No. 104014", "id_number": "CaltechAUTHORS:20150107-084235303", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150107-084235303", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY-1306125" }, { "agency": "NSF", "grant_number": "AST-1333129" }, { "agency": "NSF", "grant_number": "PHY-1440083" }, { "agency": "NSF", "grant_number": "AST-1333520" }, { "agency": "NSF", "grant_number": "PHY-1151197" }, { "agency": "Sherman Fairchild Foundation" }, { "agency": "Vincent and Beatrice Tremaine Postdoctoral Fellowship" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "Canada Research Chairs Program" }, { "agency": "Canadian Institute for Theoretical Astrophysics" }, { "agency": "NASA", "grant_number": "NNX11AC37G" }, { "agency": "NSF", "grant_number": "PHY-1402916" }, { "agency": "NSF", "grant_number": "TG-PHY100033" }, { "agency": "NSF", "grant_number": "TG-PHY990002" }, { "agency": "NSF", "grant_number": "OCI-1053575" }, { "agency": "NSF", "grant_number": "PHY-0960291" } ] }, "local_group": { "items": [ { "id": "TAPIR" } ] }, "doi": "10.1103/PhysRevD.90.104014", "primary_object": { "basename": "1405.2144v1.pdf", "url": "https://authors.library.caltech.edu/records/dd3xx-a2d03/files/1405.2144v1.pdf" }, "related_objects": [ { "basename": "PhysRevD.90.104014.pdf", "url": "https://authors.library.caltech.edu/records/dd3xx-a2d03/files/PhysRevD.90.104014.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Muhlberger, Curran D.; Nouri, Fatemeh Hossein; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/ctv49-mng79", "eprint_id": 43937, "eprint_status": "archive", "datestamp": "2023-08-19 23:11:39", "lastmod": "2023-10-26 00:01:39", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hinder-I", "name": { "family": "Hinder", "given": "Ian" } }, { "id": "Reisswig-C", "name": { "family": "Reisswig", "given": "Christian" } }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." } }, { "id": "Sperhake-U", "name": { "family": "Sperhake", "given": "Ulrich" }, "orcid": "0000-0002-3134-7088" }, { "id": "Szil\u00e1gyi-B", "name": { "family": "Szil\u00e1gyi", "given": "Bela" } }, { "id": "Zengino\u011flu-A", "name": { "family": "Zengino\u011flu", "given": "An\u0131l" } }, { "id": "Buchman-L-T", "name": { "family": "Buchman", "given": "Luisa T." } }, { "id": "Chu-Tony", "name": { "family": "Chu", "given": "Tony" } }, { "id": "Haas-R", "name": { "family": "Haas", "given": "Roland" }, "orcid": "0000-0003-1424-6178" }, { "id": "Hemberger-D-A", "name": { "family": "Hemberger", "given": "Daniel A." } }, { "id": "Lovelace-G", "name": { "family": "Lovelace", "given": "Geoffrey" }, "orcid": "0000-0002-7084-1070" }, { "id": "M\u00f6sta-P", "name": { "family": "M\u00f6sta", "given": "Philipp" }, "orcid": "0000-0002-9371-1447" }, { "id": "Taylor-N-W", "name": { "family": "Taylor", "given": "Nicholas W." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Error-analysis and comparison to analytical models of numerical waveforms produced by the NRAR Collaboration", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2014 Institute of Physics Publishing Ltd. \n\nReceived 23 July 2013, revised 29 October 2013. Published 5 December 2013. \n\nWe thank Beverly Berger and Kip Thorne for helping to establish the NRAR collaboration, Duncan Brown and Frans Pretorius for their work as members of the NRAR executive committee, Duncan Brown, Evan Ochsner and B Sathyaprakash for useful discussions in the first stage of the NRAR collaboration when the scientific plan and accuracy requirements were established. We also thank John Baker, Peter Diener, Bernard Kelly and Riccardo Sturani for useful interactions. It is also a pleasure to thank David Hilditch for useful discussions on the hyperbolicity of BSSN, Roman Gold for useful discussions on requirements for accurate\ncomputation of gravitational waves and P Ajith for help with performing and interpreting the IMRPhenom comparisons. We also thank Bruce Loftis and Christal Yost at the National\nInstitute for Computational Sciences (NICS) for their support. Caltech acknowledges support from the Sherman Fairchild Foundation and NSF grants PHY-1068881, PHY-1005655, and DMS-1065438. M Hannam was supported by Science and Technology Facilities Council grants ST/H008438/1 and ST/I001085/1. CITA acknowledges support from NSERC of Canada, the Canada Chairs Program, and the Canadian Institute for Advanced Research. Cornell acknowledges support from the Sherman Fairchild Foundation and NSF grants PHY-0969111 and PHY-1005426. FAU acknowledges financial support via the NSF grants\n0855315 and 1204334. GA Tech acknowledges financial support via NSF grants 1205864, 1212433, 0903973, 0941417, and 0955825. Jena and the AEI acknowledge financial support\nvia the DFG SFB/Transregio 7. US acknowledges financial support via the Ram\u03ccn y Cajal Programme of the Ministry of Education and Science in Spain, the FP7-PEOPLE-2011-CIG grant 293412 CBHEO, the STFC GR Roller grant ST/I002006/1, the ERC Starting grant ERC-2010-StG DyBHo, and the FP7-PEOPLE-2011-IRSES grant 295189 NRHEP. A Nerozzi acknowledges support by the Funda\u00e7\u00e3o para a Ci\u00eancia e Tecnologia through grants SFRH/BPD/47955/2008 and PTDC/FIS/116625/2010. HW acknowledges support by the ERC-2011-StG 279363\u2013HiDGR ERC Starting Grant and by the DyBHo\u2013256667 ERC Starting Grant. HW acknowledges support by FCT\u2013Portugal through grant nos. SFRH/BD/46061/2008 and CERN/FP/123593/2011 at early stages of this work. CR acknowledges financial support from NASA via the Einstein Postdoctoral Fellowship grant PF2-130099 awarded by the Chandra X-ray center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. RIT acknowledges financial support via NSF grants AST-1028087, PHY-0929114, PHY-0969855, PHY-0903782, OCI-0832606, and DRL-1136221, and NASA grant 07-ATFP07-0158. HN would also like to acknowledge support by the grand-in-aid for (24103006). UIUC acknowledges financial support via NSF grants PHY-0963136, AST-1002667, and NASA grants NNX11AE11G, NNX13AH44G. VP would also like to acknowledge financial support from a Fortner Research Fellowship. UMD acknowledges financial support via NSF grants PHY-0903631 and PHY-1208881, and NASA grants NNX09AI81G and NNX12AN10G. We also acknowledge the hospitality of the Kavli Institute for Theoretical Physics during the program 'Chirps, Mergers and Explosions' (supported by the NSF grant PHY11-25915).\nComputing time for this project was provided by the NSF on the TeraGrid (now XSEDE) systems Athena and Kraken at NICS. AEI used computational resources on the Datura cluster\nat AEI. Caltech and Cornell used additional computational resources on the Zwicky cluster at Caltech, which is supported by the Sherman Fairchild Foundation and by NSF award PHY-0960291, and on the NSF XSEDE network under grant TG-PHY990007N. CITA used additional computational resources at the SciNet HPC Consortium on the GPC system. FAU used additional computational resources via TeraGrid allocations TG-AST100021 and TGPHY100051 at NICS on the Kraken system. GA Tech used additional computational resources via XSEDE allocation TG-PHY120016, and at Georgia Tech on the Cygnus cluster. JCP used additional computational resources at the LRZ, Munich, and as part of the European PRACE petascale computing initiative on the clusters Hermit, Curie and SuperMUC; simulations were were also carried out at Advanced Research Computing (ARCCA) at Cardiff. US, AN and HW used additional computational resources via XSEDE allocation PHY-090003 at SDCS on the Trestles system and at NICS on the Kraken system, via the Barcelona Supercomputing\nCenter (BSC) allocation AECT-2012-3-0011, via the Centro de Supercomputaci\u03ccn de Galicia (CESGA) allocation ICTS-2011-234, the Baltasar-Sete-S\u03ccis cluster at CENTRA/IST Lisbon, the CANE cluster in Poland through PRACE DECI-7 and at the DiRAC HPC Facility on the COSMOS supercomputer supported by STFC and BIS. RIT used additional computational\nresources at TACC on the Ranger system via XSEDE allocation TG-PHY060027N, and at RIT on the NewHorizons/BlueSky system supported by NSF grants PHY-0722703, DMS-0820923, AST-1028087 and PHY-1229173. UIUC used additional computational resources at TACC on the Stampede system via XSEDE allocation TG-MCA99S008. Hosting for the NRAR data set and collaboration tools was provided by the Syracuse University Gravitational wave Group, supported by NSF awards PHY-0847611, PHY-1040231 and PHY-1104371. The\nEOBNRv2, SEOBNRv1, IMRPhenomB and IMRPhenomC templates were produced using the public LIGO Algorithm Library [233], while the IHES-EOB templates were produced using the public code in [234].\n\nSubmitted - 1307.5307v3.pdf
", "abstract": "The Numerical\u2013Relativity\u2013Analytical\u2013Relativity (NRAR) collaboration is a joint effort between members of the numerical relativity, analytical relativity and gravitational-wave data analysis communities. The goal of the NRAR collaboration is to produce numerical-relativity simulations of compact binaries and use them to develop accurate analytical templates for the LIGO/Virgo Collaboration to use in detecting gravitational-wave signals and extracting astrophysical information from them. We describe the results of the first stage of the NRAR project, which focused on producing an initial set of numerical waveforms from binary black holes with moderate mass ratios and spins, as well as one non-spinning binary configuration which has a mass ratio of 10. All of the numerical waveforms are analysed in a uniform and consistent manner, with numerical errors evaluated using an analysis code created by members of the NRAR collaboration. We compare previously-calibrated, non-precessing analytical waveforms, notably the effective-one-body (EOB) and phenomenological template families, to the newly-produced numerical waveforms. We find that when the binary's total mass is ~100\u2013200M_\u2299, current EOB and phenomenological models of spinning, non-precessing binary waveforms have overlaps above 99% (for advanced LIGO) with all of the non-precessing-binary numerical waveforms with mass ratios \u22644, when maximizing over binary parameters. This implies that the loss of event rate due to modelling error is below 3%. Moreover, the non-spinning EOB waveforms previously calibrated to five non-spinning waveforms with mass ratio smaller than 6 have overlaps above 99.7% with the numerical waveform with a mass ratio of 10, without even maximizing on the binary parameters.", "date": "2014-01-21", "date_type": "published", "publication": "Classical and Quantum Gravity", "volume": "31", "number": "2", "publisher": "IOP", "pagerange": "Art. No. 025012", "id_number": "CaltechAUTHORS:20140224-082418165", "issn": "0264-9381", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140224-082418165", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "National Institute for Computational Sciences (NCIS)" }, { "agency": "Sherman Fairchild Foundation" }, { "agency": "NSF", "grant_number": "PHY-1068881" }, { "agency": "NSF", "grant_number": "PHY-1005655" }, { "agency": "NSF", "grant_number": "DMS-1065438" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/H008438/1" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/I001085/1" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "Canada Chairs Program" }, { "agency": "Canadian Institute for Advanced Research (CIAR)" }, { "agency": "NSF", "grant_number": "PHY-0969111" }, { "agency": "NSF", "grant_number": "PHY-1005426" }, { "agency": "NSF", "grant_number": "0855315" }, { "agency": "NSF", "grant_number": "1204334" }, { "agency": "NSF", "grant_number": "1205864" }, { "agency": "NSF", "grant_number": "1212433" }, { "agency": "NSF", "grant_number": "0903973" }, { "agency": "NSF", "grant_number": "0941417" }, { "agency": "NSF", "grant_number": "0955825" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "SFB/Transregio 7" }, { "agency": "Ram\u03ccn y Cajal Programme" }, { "agency": "FP7-PEOPLE-2011-CIG", "grant_number": "CBHEO-293412" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/I002006/1" }, { "agency": "European Research Council (ERC)", "grant_number": "ERC-2010-StGDyBHo" }, { "agency": "FP7-PEOPLE-2011-IRSES", "grant_number": "295189 NRHEP" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e Tecnologia (FCT)", "grant_number": "SFRH/BPD/47955/2008" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e Tecnologia (FCT)", "grant_number": "PTDC/FIS/116625/2010" }, { "agency": "European Research Council (ERC)", "grant_number": "ERC-2011-StG 279363\u2013HiDGR" }, { "agency": "European Research Council (ERC)", "grant_number": "DyBHo-256667" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e Tecnologia (FCT)", "grant_number": "SFRH/BD/46061/2008" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e Tecnologia (FCT)", "grant_number": "CERN/FP/123593/2011" }, { "agency": "NASA Einstein Postdoctoral Fellowship", "grant_number": "PF2-130099" }, { "agency": "NASA", "grant_number": "NAS8-03060" }, { "agency": "NSF", "grant_number": "AST-1028087" }, { "agency": "NSF", "grant_number": "PHY-0929114" }, { "agency": "NSF", "grant_number": "PHY-0969855" }, { "agency": "NSF", "grant_number": "PHY-0903782" }, { "agency": "NSF", "grant_number": "OCI-0832606" }, { "agency": "NSF", "grant_number": "DRL-1136221" }, { "agency": "NASA", "grant_number": "07-ATFP07-0158" }, { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)", "grant_number": "24103006" }, { "agency": "NSF", "grant_number": "PHY-0963136" }, { "agency": "NSF", "grant_number": "AST-1002667" }, { "agency": "NASA", "grant_number": "NNX11AE11G" }, { "agency": "NASA", "grant_number": "NNX13AH44G" }, { "agency": "Fortner Research Fellowship" }, { "agency": "NSF", "grant_number": "PHY-0903631" }, { "agency": "NSF", "grant_number": "PHY-1208881" }, { "agency": "NASA", "grant_number": "NNX09AI81G" }, { "agency": "NASA", "grant_number": "NNX12AN10G" }, { "agency": "NSF", "grant_number": "PHY11-25915" }, { "agency": "NSF", "grant_number": "PHY-0960291" }, { "agency": "NSF", "grant_number": "PHY-990007N" }, { "agency": "NSF", "grant_number": "AST-100021" }, { "agency": "TeraGrid", "grant_number": "PHY-100051" }, { "agency": "NSF", "grant_number": "TG-PHY120016" }, { "agency": "NSF", "grant_number": "PHY-090003" }, { "agency": "Barcelona Supercomputing Center (BSC)", "grant_number": "AECT-2012-3-0011" }, { "agency": "Centro de Supercomputaci\u03ccn de Galicia (CESGA)", "grant_number": "ICTS-2011-234" }, { "agency": "NSF", "grant_number": "PHY-060027N" }, { "agency": "NSF", "grant_number": "PHY-0722703" }, { "agency": "NSF", "grant_number": "DMS-0820923" }, { "agency": "NSF", "grant_number": "AST-1028087" }, { "agency": "NSF", "grant_number": "PHY-1229173" }, { "agency": "NSF", "grant_number": "MCA-99S008" }, { "agency": "NSF", "grant_number": "PHY-0847611" }, { "agency": "NSF", "grant_number": "PHY-1040231" }, { "agency": "NSF", "grant_number": "PHY-1104371" } ] }, "doi": "10.1088/0264-9381/31/2/025012", "primary_object": { "basename": "1307.5307v3.pdf", "url": "https://authors.library.caltech.edu/records/ctv49-mng79/files/1307.5307v3.pdf" }, "resource_type": "article", "pub_year": "2014", "author_list": "Hinder, Ian; Reisswig, Christian; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/m4wdj-dzv82", "eprint_id": 43401, "eprint_status": "archive", "datestamp": "2023-08-19 22:36:09", "lastmod": "2023-10-25 23:31:08", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Le-Tiec-A", "name": { "family": "Le Tiec", "given": "Alexandre" } }, { "id": "Buonanno-A", "name": { "family": "Buonanno", "given": "Alessandra" } }, { "id": "Mrou\u00e9-A-H", "name": { "family": "Mrou\u00e9", "given": "Abdul H." } }, { "id": "Pfeiffer-H-P", "name": { "family": "Pfeiffer", "given": "Harald P." }, "orcid": "0000-0001-9288-519X" }, { "id": "Hemberger-D-A", "name": { "family": "Hemberger", "given": "Daniel A." } }, { "id": "Lovelace-G", "name": { "family": "Lovelace", "given": "Geoffrey" }, "orcid": "0000-0002-7084-1070" }, { "id": "Kidder-L-E", "name": { "family": "Kidder", "given": "Lawrence E." }, "orcid": "0000-0001-5392-7342" }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." } }, { "id": "Szil\u00e1gyi-B", "name": { "family": "Szil\u00e1gyi", "given": "Bela" } }, { "id": "Taylor-N-W", "name": { "family": "Taylor", "given": "Nicholas W." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Periastron advance in spinning black hole binaries: Gravitational self-force from numerical relativity", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2013 American Physical Society.\n\nReceived 2 September 2013; published 9 December 2013.\n\nA. B. and A. L. T. acknowledge support from NSF through Grants No. PHY-0903631 and No. PHY-1208881. A. B. also acknowledges support from NASA through Grant No. NNX09AI81G and A. L. T. from the Maryland Center for Fundamental Physics. A. M. and H. P. acknowledge support from NSERC of Canada, from the Canada Research Chairs Program, and from the Canadian Institute for Advanced Research. D. H., L. K., G. L., and S. T. acknowledge support from the Sherman Fairchild Foundation and NSF Grants No. PHY-1306125 and\nNo. PHYS-1005426 at Cornell. M. S., B. S., and N. T.\ngratefully acknowledge support from the Sherman Fairchild Foundation and NSF Grants No. PHY-1068881, No. PHY-1005655, and No. DMS-1065438 at Caltech. The numerical relativity simulations were performed at the GPC supercomputer at the SciNet HPC Consortium [65]; SciNet is funded by the Canada Foundation for Innovation (CFI) under the auspices of Compute Canada; the Government of Ontario; Ontario Research Fund\u2013Research Excellence; and the University of Toronto. Further computations were performed on the Caltech computer cluster Zwicky, which was funded by the Sherman Fairchild\nFoundation and the NSF MRI-R2 Grant No. PHY- 0960291, on SHC at Caltech, which is supported by the Sherman Fairchild Foundation, and on the NSF XSEDE network under Grant No. TG-PHY990007N.\n\nPublished - PhysRevD.88.124027.pdf
Submitted - 1309.0541v2.pdf
", "abstract": "We study the general relativistic periastron advance in spinning black hole binaries on quasicircular orbits, with spins aligned or antialigned with the orbital angular momentum, using numerical-relativity simulations, the post-Newtonian approximation, and black hole perturbation theory. By imposing a symmetry by exchange of the bodies' labels, we devise an improved version of the perturbative result and use it as the leading term of a new type of expansion in powers of the symmetric mass ratio. This allows us to measure, for the first time, the gravitational self-force effect on the periastron advance of a nonspinning particle orbiting a Kerr black hole of mass M and spin S=\u22120.5M^2, down to separations of order 9M. Comparing the predictions of our improved perturbative expansion with the exact results from numerical simulations of equal-mass and equal-spin binaries, we find a remarkable agreement over a wide range of spins and orbital separations.", "date": "2013-12-15", "date_type": "published", "publication": "Physical Review D", "volume": "88", "number": "12", "publisher": "American Physical Society", "pagerange": "Art. No. 124027", "id_number": "CaltechAUTHORS:20140116-093422080", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140116-093422080", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY-0903631" }, { "agency": "NSF", "grant_number": "PHY-1208881" }, { "agency": "NASA", "grant_number": "NNX09AI81G" }, { "agency": "NSERC (Canada)" }, { "agency": "Canada Research Chairs Program" }, { "agency": "Canadian Institute for Advanced Research" }, { "agency": "Sherman Fairchild Foundation" }, { "agency": "NSF", "grant_number": "PHY-1306125" }, { "agency": "NSF", "grant_number": "PHYS-1005426" }, { "agency": "NSF", "grant_number": "PHY-1068881" }, { "agency": "NSF", "grant_number": "PHY-1005655" }, { "agency": "NSF", "grant_number": "DMS-1065438" }, { "agency": "Maryland Center for Fundamental Physics" }, { "agency": "NSF MRI-R2", "grant_number": "PHY-0960291" }, { "agency": "NSF XSEDE", "grant_number": "TG-PHY990007N" }, { "agency": "Canada Foundation for Innovation (CFI)" }, { "agency": "Government of Ontario" }, { "agency": "Ontario Research Fund-Research Excellence" }, { "agency": "University of Toronto" }, { "agency": "Compute Canada" } ] }, "doi": "10.1103/PhysRevD.88.124027", "primary_object": { "basename": "1309.0541v2.pdf", "url": "https://authors.library.caltech.edu/records/m4wdj-dzv82/files/1309.0541v2.pdf" }, "related_objects": [ { "basename": "PhysRevD.88.124027.pdf", "url": "https://authors.library.caltech.edu/records/m4wdj-dzv82/files/PhysRevD.88.124027.pdf" } ], "resource_type": "article", "pub_year": "2013", "author_list": "Le Tiec, Alexandre; Buonanno, Alessandra; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/2kzkg-1qn50", "eprint_id": 43588, "eprint_status": "archive", "datestamp": "2023-08-19 22:34:32", "lastmod": "2023-10-25 23:41:24", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Mrou\u00e9-A-H", "name": { "family": "Mrou\u00e9", "given": "Abdul H." } }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." } }, { "id": "Szil\u00e1gyi-B", "name": { "family": "Szil\u00e1gyi", "given": "B\u00e9la" } }, { "id": "Pfeiffer-H-P", "name": { "family": "Pfeiffer", "given": "Harald P." }, "orcid": "0000-0001-9288-519X" }, { "id": "Boyle-M", "name": { "family": "Boyle", "given": "Michael" } }, { "id": "Hemberger-D-A", "name": { "family": "Hemberger", "given": "Daniel A." } }, { "id": "Kidder-L-E", "name": { "family": "Kidder", "given": "Lawrence E." }, "orcid": "0000-0001-5392-7342" }, { "id": "Lovelace-G", "name": { "family": "Lovelace", "given": "Geoffrey" }, "orcid": "0000-0002-7084-1070" }, { "id": "Ossokine-S", "name": { "family": "Ossokine", "given": "Serguei" } }, { "id": "Taylor-N-W", "name": { "family": "Taylor", "given": "Nicholas W." } }, { "id": "Zengino\u011flu-A", "name": { "family": "Zengino\u011flu", "given": "An\u0131l" } }, { "id": "Buchman-L-T", "name": { "family": "Buchman", "given": "Luisa T." } }, { "id": "Chu-T", "name": { "family": "Chu", "given": "Tony" } }, { "id": "Foley-E", "name": { "family": "Foley", "given": "Evan" } }, { "id": "Giesler-M-D", "name": { "family": "Giesler", "given": "Matthew" }, "orcid": "0000-0003-2300-893X" }, { "id": "Owen-R", "name": { "family": "Owen", "given": "Robert" } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Catalog of 174 Binary Black Hole Simulations for Gravitational Wave Astronomy", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2013 American Physical Society.\n\nReceived 27 May 2013; revised 5 September 2013; published 11 December 2013.\n\nWe thank Christian Ott and Kip Thorne for helpful discussions. This work was supported in part by NSERC of Canada, the Canada Chairs Program, and the Canadian Institute for Advanced Research; the Sherman Fairchild Foundation; and NSF Grants No. PHY-0969111 and No. PHY-1005426 at Cornell, NSF Grants No. PHY-1068881, No. PHY-1005655, and No. DMS-1065438 at Caltech, and NSF Grant No. PHY-1307489 at Cal State Fullerton. Simulations used in this work were computed with the SpEC code [27]. Computations were performed on the Zwicky cluster at Caltech, which is supported by the Sherman Fairchild Foundation and by NSF Grant No. PHY-0960291; on the NSF XSEDE network under Grant No. TG-PHY990007N; on the Orca Cluster supported by Cal State Fullerton; and on the GPC Supercomputer at the SciNet HPC Consortium [78]. SciNet is funded by the Canada Foundation for Innovation under the auspices of Compute Canada, the Government of Ontario, Ontario Research Fund\u2014Research Excellence, and the University of Toronto.\n\nPublished - PhysRevLett.111.241104.pdf
Submitted - 1304.6077v3.pdf
", "abstract": "This Letter presents a publicly available catalog of 174 numerical binary black hole simulations following up to 35 orbits. The catalog includes 91 precessing binaries, mass ratios up to 8:1, orbital eccentricities from a few percent to 10^(-5), black hole spins up to 98% of the theoretical maximum, and radiated energies up to 11.1% of the initial mass. We establish remarkably good agreement with post-Newtonian precession of orbital and spin directions for two new precessing simulations, and we discuss other applications of this catalog. Formidable challenges remain: e.g., precession complicates the connection of numerical and approximate analytical waveforms, and vast regions of the parameter space remain unexplored.", "date": "2013-12-11", "date_type": "published", "publication": "Physical Review Letters", "volume": "111", "number": "24", "publisher": "American Physical Society", "pagerange": "Article No. 241104", "id_number": "CaltechAUTHORS:20140130-135558192", "issn": "0031-9007", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140130-135558192", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "Canada Chairs Program" }, { "agency": "Canadian Institute for Advanced Research (CIAR)" }, { "agency": "Sherman Fairchild Foundation" }, { "agency": "NSF", "grant_number": "PHY-0969111" }, { "agency": "NSF", "grant_number": "PHY-1005426" }, { "agency": "NSF", "grant_number": "PHY-1068881" }, { "agency": "NSF", "grant_number": "PHY-1005655" }, { "agency": "NSF", "grant_number": "DMS-1065438" }, { "agency": "NSF", "grant_number": "PHY-1307489" }, { "agency": "NSF", "grant_number": "PHY-0960291" }, { "agency": "NSF", "grant_number": "TG-PHY990007N" }, { "agency": "Cal State Fullerton" }, { "agency": "Canada Foundation for Innovation (CFI)" }, { "agency": "Compute Canada" }, { "agency": "Government of Ontario" }, { "agency": "Ontario Research Fund-Research Excellence" }, { "agency": "University of Toronto" } ] }, "doi": "10.1103/PhysRevLett.111.241104", "primary_object": { "basename": "1304.6077v3.pdf", "url": "https://authors.library.caltech.edu/records/2kzkg-1qn50/files/1304.6077v3.pdf" }, "related_objects": [ { "basename": "PhysRevLett.111.241104.pdf", "url": "https://authors.library.caltech.edu/records/2kzkg-1qn50/files/PhysRevLett.111.241104.pdf" } ], "resource_type": "article", "pub_year": "2013", "author_list": "Mrou\u00e9, Abdul H.; Scheel, Mark A.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/sv8a6-vzw29", "eprint_id": 42416, "eprint_status": "archive", "datestamp": "2023-08-19 21:50:33", "lastmod": "2023-10-25 16:01:37", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hinderer-T", "name": { "family": "Hinderer", "given": "Tanja" }, "orcid": "0000-0002-3394-6105" }, { "id": "Buonanno-A", "name": { "family": "Buonanno", "given": "Alessandra" } }, { "id": "Mrou\u00e9-A-H", "name": { "family": "Mrou\u00e9", "given": "Abdul H." } }, { "id": "Hemberger-D-A", "name": { "family": "Hemberger", "given": "Daniel A." } }, { "id": "Lovelace-G", "name": { "family": "Lovelace", "given": "Geoffrey" }, "orcid": "0000-0002-7084-1070" }, { "id": "Pfeiffer-H-P", "name": { "family": "Pfeiffer", "given": "Harald P." }, "orcid": "0000-0001-9288-519X" }, { "id": "Kidder-L-E", "name": { "family": "Kidder", "given": "Lawrence E." }, "orcid": "0000-0001-5392-7342" }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." } }, { "id": "Szil\u00e1gyi-B", "name": { "family": "Szil\u00e1gyi", "given": "B\u00e9la" } }, { "id": "Taylor-N-W", "name": { "family": "Taylor", "given": "Nicholas W." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Periastron advance in spinning black hole binaries: comparing effective-one-body and numerical relativity", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2013 American Physical Society.\n\nReceived 3 September 2013; published 4 October 2013.\n\nWe thank Andrea Taracchini and Yi Pan for help with implementing the EOB Hamiltonian and Enrico Barausse, Alexandre Le Tiec, Yi Pan and Andrea Taracchini for useful interactions and comments. A. B. acknowledges partial support from NSF Grants No. PHY-0903631 and No. PHY-1208881, and NASA Grant No. NNX09AI81G. T. H. acknowledges support from NSF Grants No. PHY-0903631 and No. PHY-1208881 and the Maryland Center for Fundamental Physics. A. M. and H. P. acknowledge support from NSERC of Canada, from the Canada Research Chairs Program, and from the Canadian Institute for Advanced Research. We acknowledge support from the Sherman Fairchild Foundation, from NSF Grants No. PHY-0969111 and No. PHYS-1005426 at Cornell, and from NSF Grants No. PHY-1068881 and No. PHY-\n1005655 at Caltech. The numerical-relativity simulations\nwere performed at the GPC supercomputer at the SciNet\nHPC Consortium [95]; SciNet is funded by the Canada\nFoundation for Innovation (CFI) under the auspices of\nCompute Canada; the Government of Ontario; Ontario\nResearch Fund\u2014Research Excellence; and the University\nof Toronto. Further computations were performed on\nthe Caltech computer cluster Zwicky, which is funded\nby the Sherman Fairchild Foundation and the NSF MRI-R2 Grant No. PHY-0960291, on SHC at Caltech, which is supported by the Sherman Fairchild Foundation, and on the NSF XSEDE network under Grant No. TG-PHY990007N.\n\nPublished - PhysRevD.88.084005.pdf
Submitted - 1309.0544v2.pdf
", "abstract": "We compute the periastron advance using the effective-one-body formalism for binary black holes moving on quasicircular orbits and having spins collinear with the orbital angular momentum. We compare the predictions with the periastron advance recently computed in accurate numerical-relativity simulations and find remarkable agreement for a wide range of spins and mass ratios. These results do not use any numerical-relativity calibration of the effective-one-body model, and stem from two key ingredients in the effective-one-body Hamiltonian: (i) the mapping of the two-body dynamics of spinning particles onto the dynamics of an effective spinning particle in a (deformed) Kerr spacetime, fully symmetrized with respect to the two-body masses and spins, and (ii) the resummation, in the test-particle limit, of all post-Newtonian corrections linear in the spin of the particle. In fact, even when only the leading spin post-Newtonian corrections are included in the effective-one-body spinning Hamiltonian but all the test-particle corrections linear in the spin of the particle are resummed we find very good agreement with the numerical results (within the numerical error for equal-mass binaries and discrepancies of at most 1% for larger mass ratios). Furthermore, we specialize to the extreme mass-ratio limit and derive, using the equations of motion in the gravitational skeleton approach, analytical expressions for the periastron advance, the meridional Lense-Thirring precession and spin precession frequency in the case of a spinning particle on a nearly circular equatorial orbit in Kerr spacetime, including also terms quadratic in the spin.", "date": "2013-10-04", "date_type": "published", "publication": "Physical Review D", "volume": "88", "number": "8", "publisher": "American Physical Society", "pagerange": "Art. No. 084005", "id_number": "CaltechAUTHORS:20131113-094821753", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20131113-094821753", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY-0903631" }, { "agency": "NSF", "grant_number": "PHY-1208881" }, { "agency": "NASA", "grant_number": "NNX09AI81G" }, { "agency": "NSF", "grant_number": "PHY-0903631" }, { "agency": "NSF", "grant_number": "PHY-1208881" }, { "agency": "Maryland Center for Fundamental Physics" }, { "agency": "NSERC (Canada)" }, { "agency": "Canada Research Chairs Program" }, { "agency": "Canadian Institute for Advanced Research (CIAR)" }, { "agency": "Sherman Fairchild Foundation" }, { "agency": "NSF", "grant_number": "PHY-0969111" }, { "agency": "NSF", "grant_number": "PHYS-1005426" }, { "agency": "NSF", "grant_number": "PHY-1068881" }, { "agency": "NSF", "grant_number": "PHY-1005655" }, { "agency": "NSF MRI-R2", "grant_number": "PHY-0960291" }, { "agency": "NSF XSEDE network", "grant_number": "TG-PHY990007N" }, { "agency": "Canada Foundation for Innovation (CFI)" }, { "agency": "Compute Canada" }, { "agency": "Government of Ontario" }, { "agency": "Ontario Research Fund-Research Excellence" }, { "agency": "University of Toronto" } ] }, "doi": "10.1103/PhysRevD.88.084005", "primary_object": { "basename": "1309.0544v2.pdf", "url": "https://authors.library.caltech.edu/records/sv8a6-vzw29/files/1309.0544v2.pdf" }, "related_objects": [ { "basename": "PhysRevD.88.084005.pdf", "url": "https://authors.library.caltech.edu/records/sv8a6-vzw29/files/PhysRevD.88.084005.pdf" } ], "resource_type": "article", "pub_year": "2013", "author_list": "Hinderer, Tanja; Buonanno, Alessandra; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/n8q8j-ad619", "eprint_id": 41706, "eprint_status": "archive", "datestamp": "2023-08-19 21:24:08", "lastmod": "2023-10-25 14:40:30", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hemberger-D-A", "name": { "family": "Hemberger", "given": "Daniel A." } }, { "id": "Lovelace-G", "name": { "family": "Lovelace", "given": "Geoffrey" }, "orcid": "0000-0002-7084-1070" }, { "id": "Loredo-T-J", "name": { "family": "Loredo", "given": "Thomas J." }, "orcid": "0000-0003-4692-4607" }, { "id": "Kidder-L-E", "name": { "family": "Kidder", "given": "Lawrence E." }, "orcid": "0000-0001-5392-7342" }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." } }, { "id": "Szil\u00e1gyi-B", "name": { "family": "Szil\u00e1gyi", "given": "B\u00e9la" } }, { "id": "Taylor-N-W", "name": { "family": "Taylor", "given": "Nicholas W." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Final spin and radiated energy in numerical simulations of binary black holes with equal masses and equal, aligned or antialigned spins", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2013 American Physical Society.\n\nReceived 28 May 2013; published 5 September 2013.\n\nWe thank Matt Giesler, Tony Chu, and Bryant Garcia for\nproviding data from their simulations. We gratefully\nacknowledge support from the Sherman Fairchild\nFoundation; from NSF Grants No. PHY-0969111 and\nNo. PHY-1005426 at Cornell; and from NSF Grants\nNo. PHY-1068881, No. PHY-1005655, and No. DMS-\n1065438 at Caltech. The work of T. J. L. for this project\nwas supported by NSF Grant No. AST-0908439 and NASA\nGrant No. NNX09AK60G. Simulations used in this work\nwere computed with SpEC [32]. Computations were performed\non SHC at Caltech, which is supported by the\nSherman Fairchild Foundation; on the Zwicky cluster at\nCaltech, which is supported by the Sherman Fairchild\nFoundation and by NSF Award No. PHY-0960291; on the\nNSF XSEDE network under Grant No. TG-PHY990007N;\nand on the GPC supercomputer at the SciNet HPC\nConsortium [68]. SciNet is funded by the following: the\nCanada Foundation for Innovation under the auspices of\nCompute Canada, the Government of Ontario, Ontario\nResearch Fund-Research Excellence, and the University\nof Toronto.\n\nPublished - PhysRevD.88.064014.pdf
Submitted - 1305.5991v2.pdf
", "abstract": "The behavior of merging black holes (including the emitted gravitational waves and the properties of the remnant) can currently be computed only by numerical simulations. This paper introduces ten numerical relativity simulations of binary black holes with equal masses and equal spins aligned or antialigned with the orbital angular momentum. The initial spin magnitudes have |\u03c7_i|\u22720.95 and are more concentrated in the aligned direction because of the greater astrophysical interest of this case. We combine these data with five previously reported simulations of the same configuration, but with different spin magnitudes, including the highest spin simulated to date, \u03c7_i\u22480.97. This data set is sufficiently accurate to enable us to offer improved analytic fitting formulas for the final spin and for the energy radiated by gravitational waves as a function of initial spin. The improved fitting formulas can help to improve our understanding of the properties of binary black hole merger remnants and can be used to enhance future approximate waveforms for gravitational wave searches, such as effective-one-body waveforms.", "date": "2013-09-05", "date_type": "published", "publication": "Physical Review D", "volume": "88", "number": "6", "publisher": "American Physical Society", "pagerange": "Art. No. 064014", "id_number": "CaltechAUTHORS:20131007-103434116", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20131007-103434116", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Sherman Fairchild Foundation" }, { "agency": "NSF", "grant_number": "PHY-0969111" }, { "agency": "NSF", "grant_number": "PHY-1005426" }, { "agency": "NSF", "grant_number": "PHY-1068881" }, { "agency": "NSF", "grant_number": "PHY-1005655" }, { "agency": "NSF", "grant_number": "DMS-1065438" }, { "agency": "NSF", "grant_number": "AST-0908439" }, { "agency": "NASA", "grant_number": "NNX09AK60G" }, { "agency": "NSF", "grant_number": "PHY-0960291" }, { "agency": "NSF", "grant_number": "TG-PHY990007N" }, { "agency": "Canada Foundation for Innovation" }, { "agency": "Government of Ontario" }, { "agency": "Ontario Research Fund-Research Excellence" }, { "agency": "University of Toronto" }, { "agency": "Compute Canada" } ] }, "local_group": { "items": [ { "id": "TAPIR" } ] }, "doi": "10.1103/PhysRevD.88.064014", "primary_object": { "basename": "1305.5991v2.pdf", "url": "https://authors.library.caltech.edu/records/n8q8j-ad619/files/1305.5991v2.pdf" }, "related_objects": [ { "basename": "PhysRevD.88.064014.pdf", "url": "https://authors.library.caltech.edu/records/n8q8j-ad619/files/PhysRevD.88.064014.pdf" } ], "resource_type": "article", "pub_year": "2013", "author_list": "Hemberger, Daniel A.; Lovelace, Geoffrey; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/9aq56-dkj61", "eprint_id": 39018, "eprint_status": "archive", "datestamp": "2023-08-19 20:23:42", "lastmod": "2023-10-24 14:58:12", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hemberger-D-A", "name": { "family": "Hemberger", "given": "Daniel A." } }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." } }, { "id": "Kidder-L-E", "name": { "family": "Kidder", "given": "Lawrence E." }, "orcid": "0000-0001-5392-7342" }, { "id": "Szil\u00e1gyi-B", "name": { "family": "Szil\u00e1gyi", "given": "B\u00e9la" } }, { "id": "Lovelace-G", "name": { "family": "Lovelace", "given": "Geoffrey" }, "orcid": "0000-0002-7084-1070" }, { "id": "Taylor-N-W", "name": { "family": "Taylor", "given": "Nicholas W." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Dynamical excision boundaries in spectral evolutions of binary black hole spacetimes", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2013 IOP Publishing Ltd. \n\nReceived 17 December 2012, in final form 5 April 2013. Published 25 April 2013. \n\nWe would like to thank Harald Pfeiffer for useful discussions. We would like to thank Abdul Mrou\u00e9 for performing simulations that led to the development and improvement of some of the mappings presented in this paper. We gratefully acknowledge support from the Sherman Fairchild Foundation; from NSF grants PHY-0969111 and PHY-1005426 at Cornell, and from NSF grants PHY-1068881 and PHY-1005655 at Caltech. Simulations used in this work\nwere computed with the SpEC code [17]. Computations were performed on the Zwicky cluster at Caltech, which is supported by the Sherman Fairchild Foundation and by NSF award PHY-0960291; on the NSF XSEDE network under grant TG-PHY990007N; and on the GPC supercomputer at the SciNet HPC Consortium [29]. SciNet is funded by: the Canada Foundation for Innovation under the auspices of Compute Canada; the Government of Ontario; Ontario Research Fund\u2013Research Excellence; and the University of Toronto.\n\nSubmitted - 1211.6079.pdf
", "abstract": "Simulations of binary black hole systems using the Spectral Einstein Code (SpEC) are done on a computational domain that excises the regions inside the black holes. It is imperative that the excision boundaries are outflow boundaries with respect to the hyperbolic evolution equations used in the simulation. We employ a time-dependent mapping between the fixed computational frame and the inertial frame through which the black holes move. The time-dependent parameters of the mapping are adjusted throughout the simulation by a feedback control system in order to follow the motion of the black holes, to adjust the shape and size of the excision surfaces so that they remain outflow boundaries, and to prevent large distortions of the grid. We describe in detail the mappings and control systems that we use. We show how these techniques have been essential in the evolution of binary black hole systems with extreme configurations, such as large spin magnitudes and high mass ratios, especially during the merger, when apparent horizons are highly distorted and the computational domain becomes compressed. The techniques introduced here may be useful in other applications of partial differential equations that involve time-dependent mappings.", "date": "2013-06-07", "date_type": "published", "publication": "Classical and Quantum Gravity", "volume": "30", "number": "11", "publisher": "IOP", "pagerange": "Art. No. 115001", "id_number": "CaltechAUTHORS:20130621-091719465", "issn": "0264-9381", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130621-091719465", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY-0969111" }, { "agency": "NSF", "grant_number": "PHY-1005426" }, { "agency": "NSF", "grant_number": "PHY-1068881" }, { "agency": "NSF", "grant_number": "PHY-1005655" }, { "agency": "Sherman Fairchild Foundation" }, { "agency": "NSF", "grant_number": "PHY-0960291" }, { "agency": "NSF", "grant_number": "TG-PHY990007N" }, { "agency": "Canada Foundation for Innovation" }, { "agency": "Government of Ontario" }, { "agency": "Ontario Research Fund\u2013Research Excellence" }, { "agency": "University of Toronto" } ] }, "local_group": { "items": [ { "id": "TAPIR" } ] }, "doi": "10.1088/0264-9381/30/11/115001", "primary_object": { "basename": "1211.6079.pdf", "url": "https://authors.library.caltech.edu/records/9aq56-dkj61/files/1211.6079.pdf" }, "resource_type": "article", "pub_year": "2013", "author_list": "Hemberger, Daniel A.; Scheel, Mark A.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/7fn1x-naf88", "eprint_id": 38303, "eprint_status": "archive", "datestamp": "2023-08-19 19:29:07", "lastmod": "2023-10-23 20:01:57", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Foucart-F", "name": { "family": "Foucart", "given": "Francois" }, "orcid": "0000-0003-4617-4738" }, { "id": "Deaton-M-B", "name": { "family": "Deaton", "given": "M. Brett" } }, { "id": "Duez-M-D", "name": { "family": "Duez", "given": "Matthew D." }, "orcid": "0000-0002-0050-1783" }, { "id": "Kidder-L-E", "name": { "family": "Kidder", "given": "Lawrence E." }, "orcid": "0000-0001-5392-7342" }, { "id": "MacDonald-I", "name": { "family": "MacDonald", "given": "Ilana" } }, { "id": "Ott-C-D", "name": { "family": "Ott", "given": "Christian D." }, "orcid": "0000-0003-4993-2055" }, { "id": "Pfeiffer-H-P", "name": { "family": "Pfeiffer", "given": "Harald P." }, "orcid": "0000-0001-9288-519X" }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." } }, { "id": "Szil\u00e1gyi-B", "name": { "family": "Szil\u00e1gyi", "given": "B\u00e9la" } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Black-hole\u2013neutron-star mergers at realistic mass ratios: Equation of state and spin orientation effects", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2013 American Physical Society. \n\nReceived 23 December 2012; published 2 April 2013. \n\nThe authors wish to thank Kipp Cannon, Michael Boyle, and Tanja Hinderer for useful discussions and suggestions over the course of this project; Nicolas Smith-Lefebvre for computing and providing LIGO noise curves tuned to high frequency; the members of the SXS Collaboration for their regular suggestions; and the participants of the \"Rattle and Shine\" workshop at KITP (Santa Barbara) for stimulating discussions relevant to this work. We thank Patrick Fraser for assistance with generating Figs. 1 and 2 and John Wendell for assistance with the other figures. M. D. D. acknowledges support through NASA Grant No. NNX11AC37G and NSF Grant No. PHY-1068243. H. P. P. gratefully acknowledges support from the NSERC of Canada, from the Canada Research Chairs Program, and from the Canadian Institute for Advanced Research. L. E. K. and S. A. T. gratefully acknowledge support from the Sherman Fairchild Foundation, and from NSF Grants No. PHY-0969111 and No. PHY-1005426. C.D. O., M. A. S., and B. S. are partially supported by NASA ATP Grant No. NNX11AC37G and NSF Grants No. PHY-1151197, No. PHY-1068881, and No. PHY-1005655, by the Sherman Fairchild Foundation, and the Alfred P. Sloan Foundation. F. F., L. E. K., and M. A. S. were partially supported by the National Science Foundation under Grant No. NSF PHY11-25915. Computations were performed on the GPC supercomputer at the SciNet HPC Consortium [88] funded by the Canada Foundation for Innovation, the Government of Ontario, Ontario Research Fund-Research Excellence, and the University of Toronto; on Briar\u00e9e from University of Montreal, under the administration of Calcul Qubec and Compute Canada, supported by Canadian Foundation for Innovation (CFI), Natural Sciences and Engineering Research Council of Canada (NSERC), NanoQu\u00e9bec, RMGA and the Fonds de recherche du Qu\u00e9bec-Nature et technologies (FRQ-NT); and on the Zwicky cluster at Caltech, supported by the Sherman Fairchild Foundation and by NSF Grant No. PHY-0960291. This work also used the Extreme Science and Engineering Discovery Environment (XSEDE), which is supported by National Science Foundation Grant No. OCI-1053575.\n\nPublished - PhysRevD.87.084006.pdf
Submitted - 1212.4810.pdf
", "abstract": "Black-hole\u2013neutron-star mergers resulting in the disruption of the neutron star and the formation of an accretion disk and/or the ejection of unbound material are prime candidates for the joint detection of gravitational-wave and electromagnetic signals when the next generation of gravitational-wave detectors comes online. However, the disruption of the neutron star and the properties of the postmerger remnant are very sensitive to the parameters of the binary (mass ratio, black-hole spin, neutron star radius). In this paper, we study the impact of the radius of the neutron star and the alignment of the black-hole spin on black-hole\u2013neutron-star mergers within the range of mass ratio currently deemed most likely for field binaries (M_BH\u223c7M_NS) and for black-hole spins large enough for the neutron star to disrupt (J_BH/M^(2)_(BH)=0.9). We find that (i) In this regime, the merger is particularly sensitive to the radius of the neutron star, with remnant masses varying from 0.3M_NS to 0.1M_NS for changes of only 2 km in the NS radius; (ii) 0.01M_(\u2299)\u20130.05M_(\u2299) of unbound material can be ejected with kinetic energy \u227310^(51)\u2009\u2009ergs, a significant increase compared to low mass ratio, low spin binaries. This ejecta could power detectable postmerger optical and radio afterglows. (iii) Only a small fraction of the Advanced LIGO events in this parameter range have gravitational-wave signals which could offer constraints on the equation of state of the neutron star (at best \u223c3% of the events for a single detector at design sensitivity). (iv) A misaligned black-hole spin works against disk formation, with less neutron-star material remaining outside of the black hole after merger, and a larger fraction of that material remaining in the tidal tail instead of the forming accretion disk. (v) Large kicks v_kick\u2273300\u2009\u2009km/s can be given to the final black hole as a result of a precessing black-hole\u2013neutron-star merger, when the disruption of the neutron star occurs just outside or within the innermost stable spherical orbit.", "date": "2013-04-02", "date_type": "published", "publication": "Physical Review D", "volume": "87", "number": "8", "publisher": "American Physical Society", "pagerange": "Art. No. 084006", "id_number": "CaltechAUTHORS:20130506-154544306", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130506-154544306", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNX11AC37G" }, { "agency": "NSF", "grant_number": "PHY-1068243" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "Canada Research Chairs Program" }, { "agency": "Canadian Institute for Advanced Research (CIFAR)" }, { "agency": "Sherman Fairchild Foundation" }, { "agency": "NSF", "grant_number": "PHY-0969111" }, { "agency": "NSF", "grant_number": "PHY-1005426" }, { "agency": "NASA", "grant_number": "NNX11AC37G" }, { "agency": "NSF", "grant_number": "PHY-1151197" }, { "agency": "NSF", "grant_number": "PHY-1068881" }, { "agency": "NSF", "grant_number": "PHY-1005655" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "NSF", "grant_number": "PHY11-25915" } ] }, "local_group": { "items": [ { "id": "TAPIR" } ] }, "doi": "10.1103/PhysRevD.87.084006", "primary_object": { "basename": "1212.4810.pdf", "url": "https://authors.library.caltech.edu/records/7fn1x-naf88/files/1212.4810.pdf" }, "related_objects": [ { "basename": "PhysRevD.87.084006.pdf", "url": "https://authors.library.caltech.edu/records/7fn1x-naf88/files/PhysRevD.87.084006.pdf" } ], "resource_type": "article", "pub_year": "2013", "author_list": "Foucart, Francois; Deaton, M. Brett; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/a0npp-9cc58", "eprint_id": 35750, "eprint_status": "archive", "datestamp": "2023-08-19 13:15:54", "lastmod": "2023-10-20 20:36:30", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Garcia-B", "name": { "family": "Garcia", "given": "Bryant" } }, { "id": "Lovelace-G", "name": { "family": "Lovelace", "given": "Geoffrey" }, "orcid": "0000-0002-7084-1070" }, { "id": "Kidder-L-E", "name": { "family": "Kidder", "given": "Lawrence E." }, "orcid": "0000-0001-5392-7342" }, { "id": "Boyle-M", "name": { "family": "Boyle", "given": "Michael" } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." } }, { "id": "Szil\u00e1gyi-B", "name": { "family": "Szilagyi", "given": "Bela" } } ] }, "title": "Are different approaches to constructing initial data for binary black hole simulations of the same astrophysical situation equivalent?", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2012 American Physical Society. \n\nReceived 14 June 2012; published 31 October 2012. \n\nWe are pleased to thank Harald Pfeiffer for helpful discussions. This work was supported in part by the Sherman Fairchild Foundation, by NSF Grants No. PHY-0969111 and No. PHY-1005426 at Cornell, No. PHY-1068881 and No. PHY-1005655 at Caltech, and by NASA Grant No. NNX09AF96G. The new numerical computations presented in this paper were performed primarily on the Caltech computer cluster \"Zwicky,\" which was funded by the Sherman Fairchild Foundation and the NSF MRI-R2 Grant No. PHY-0960291 to Caltech.\n\nPublished - PhysRevD.86.084054.pdf
Submitted - 1206.2943.pdf
", "abstract": "Initial data for numerical evolutions of binary-black holes have been dominated by \"conformally flat\" (CF) data (i.e., initial data where the conformal background metric is chosen to be flat) because they are easy to construct. However, CF initial data cannot simulate nearly extremal spins, while more complicated \"conformally curved\" initial data (i.e., initial data in which the background metric is not explicitly chosen to be flat), such as initial data where the spatial metric is chosen to be proportional to a weighted superposition of two Kerr-Schild black holes can. Here we establish the consistency between the astrophysical results of these two initial data schemes for nonspinning binary systems. We evolve the inspiral, merger, and ringdown of two equal-mass, nonspinning black holes using superposed Kerr-Schild initial data and compare with an analogous simulation using CF initial data. We find that the resultant gravitational-waveform phases agree to within \u03b4\u03d5\u227210^(-2) radians and the amplitudes agree to within \u03b4A/A\u22725\u00d710^(-3), which are within the numerical errors of the simulations. Furthermore, we find that the final mass and spin of the remnant black hole agree to one part in 10^5.", "date": "2012-10-31", "date_type": "published", "publication": "Physical Review D", "volume": "86", "number": "8", "publisher": "American Physical Society", "pagerange": "Art. No. 084054", "id_number": "CaltechAUTHORS:20121130-131737755", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20121130-131737755", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Sherman Fairchild Foundation" }, { "agency": "NSF", "grant_number": "PHY-0969111" }, { "agency": "NSF", "grant_number": "PHY-1005426" }, { "agency": "NSF", "grant_number": "PHY-1068881" }, { "agency": "NSF", "grant_number": "PHY-1005655" }, { "agency": "NASA", "grant_number": "NNX09AF96G" }, { "agency": "NSF", "grant_number": "PHY-0960291" } ] }, "local_group": { "items": [ { "id": "TAPIR" } ] }, "doi": "10.1103/PhysRevD.86.084054", "primary_object": { "basename": "1206.2943.pdf", "url": "https://authors.library.caltech.edu/records/a0npp-9cc58/files/1206.2943.pdf" }, "related_objects": [ { "basename": "PhysRevD.86.084054.pdf", "url": "https://authors.library.caltech.edu/records/a0npp-9cc58/files/PhysRevD.86.084054.pdf" } ], "resource_type": "article", "pub_year": "2012", "author_list": "Garcia, Bryant; Lovelace, Geoffrey; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/p6q7d-aqq54", "eprint_id": 29581, "eprint_status": "archive", "datestamp": "2023-08-19 09:53:38", "lastmod": "2023-10-24 22:18:55", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Foucart-F", "name": { "family": "Foucart", "given": "Francois" }, "orcid": "0000-0003-4617-4738" }, { "id": "Duez-M-D", "name": { "family": "Duez", "given": "Matthew D." }, "orcid": "0000-0002-0050-1783" }, { "id": "Kidder-L-E", "name": { "family": "Kidder", "given": "Lawrence E." }, "orcid": "0000-0001-5392-7342" }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." } }, { "id": "Szil\u00e1gyi-B", "name": { "family": "Szilagyi", "given": "Bela" } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Black hole-neutron star mergers for 10 M_\u2609 black holes", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2012 American Physical Society. \n\nReceived 7 November 2011; published 7 February 2012. \n\nWe thank Dan Hemberger, Jeff Kaplan, Geoffrey Lovelace, Curran Muhlberger, and Harald Pfeiffer for useful discussions and suggestions. This work was supported in part by a grant from the Sherman Fairchild Foundation; by NSF Grants No. PHY-0969111 and No. PHY-1005426 and NASA Grant No. NNX09AF96G at Cornell; and by NSF Grants No. PHY-0601459, No. PHY-1068881, and No. PHY-1005655, and NASA Grant No. NNX09AF97G at Caltech. M. D. acknowledges support through NASA Grant No. NNX11AC37G and NSF Grant No. PHY-1068243. This research was supported in part by the NSF through TeraGrid [50] resources provided by NCSA's Lonestar cluster under Grant No. TG-PHY990007N. Computations were also performed on the Caltech compute cluster Zwicky, funded by NSF MRI Grant No. PHY-0960291, and on the GPC supercomputer at the SciNet HPC Consortium. SciNet is funded by the Canada Foundation for Innovation under the auspices of Compute Canada, the Government of Ontario; Ontario Research Fund-Research Excellence, and the University of Toronto.\n\nPublished - Foucart2012p17343Phys_Rev_D.pdf
Submitted - 1111.1677.pdf
", "abstract": "General relativistic simulations of black hole-neutron star mergers have currently been limited to low-mass black holes (M_(BH)\u22647\u2009\u2009M_\u2299), even though population synthesis models indicate that a majority of mergers might involve more massive black holes (M_(BH)\u226510\u2009\u2009M_\u2299). We present the first general relativistic simulations of black hole-neutron star mergers with M_(BH_\u223c10\u2009\u2009M_\u2299. For massive black holes, the tidal forces acting on the neutron star are usually too weak to disrupt the star before it reaches the innermost stable circular orbit of the black hole. Varying the spin of the black hole in the range \u03b1_(BH)/M_(BH)=0.5\u20130.9, we find that mergers result in the disruption of the star and the formation of a massive accretion disk only for large spins \u03b1_(BH)/M_(BH)\u22650.7\u20130.9. From these results, we obtain updated constraints on the ability of black hole-neutron star mergers to be the progenitors of short gamma-ray bursts as a function of the mass and spin of the black hole. We also discuss the dependence of the gravitational wave signal on the black hole parameters, and provide waveforms and spectra from simulations beginning 7\u20138 orbits before the merger.", "date": "2012-02-07", "date_type": "published", "publication": "Physical Review D", "volume": "85", "number": "4", "publisher": "American Physical Society", "pagerange": "Art. No. 044015", "id_number": "CaltechAUTHORS:20120306-070840141", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120306-070840141", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Sherman Fairchild Foundation" }, { "agency": "NSF", "grant_number": "PHY-0969111" }, { "agency": "NSF", "grant_number": "PHY-1005426" }, { "agency": "NASA", "grant_number": "NNX09AF96G" }, { "agency": "NSF", "grant_number": "PHY-0601459" }, { "agency": "NSF", "grant_number": "PHY-1068881" }, { "agency": "NSF", "grant_number": "PHY-1005655" }, { "agency": "NASA", "grant_number": "NNX09AF97G" }, { "agency": "NASA", "grant_number": "NNX11AC37G" }, { "agency": "NSF", "grant_number": "PHY-1068243" }, { "agency": "NSF", "grant_number": "TG-PHY990007N" }, { "agency": "NSF", "grant_number": "PHY-0960291" }, { "agency": "Canada Foundation for Innovation" } ] }, "local_group": { "items": [ { "id": "TAPIR" } ] }, "doi": "10.1103/PhysRevD.85.044015", "primary_object": { "basename": "1111.1677.pdf", "url": "https://authors.library.caltech.edu/records/p6q7d-aqq54/files/1111.1677.pdf" }, "related_objects": [ { "basename": "Foucart2012p17343Phys_Rev_D.pdf", "url": "https://authors.library.caltech.edu/records/p6q7d-aqq54/files/Foucart2012p17343Phys_Rev_D.pdf" } ], "resource_type": "article", "pub_year": "2012", "author_list": "Foucart, Francois; Duez, Matthew D.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/cmnqz-wqt62", "eprint_id": 22588, "eprint_status": "archive", "datestamp": "2023-08-19 05:13:59", "lastmod": "2023-10-23 17:02:11", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Foucart-F", "name": { "family": "Foucart", "given": "Francois" }, "orcid": "0000-0003-4617-4738" }, { "id": "Duez-M-D", "name": { "family": "Duez", "given": "Matthew D." }, "orcid": "0000-0002-0050-1783" }, { "id": "Kidder-L-E", "name": { "family": "Kidder", "given": "Lawrence E." }, "orcid": "0000-0001-5392-7342" }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Black hole-neutron star mergers: Effects of the orientation of the black hole spin", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2011 American Physical Society. \n\nReceived 23 July 2010; published 6 January 2011. \n\nWe thank Geoffrey Lovelace and Harald Pfeiffer for useful discussions and suggestions. This work was supported in part by a grant from the Sherman Fairchild Foundation, by NSF Grants Nos. PHY-0652952 and PHY-0652929, and NASA Grant No. NNX09AF96G. This research was supported in part by the NSF through TeraGrid [42] resources provided by NCSA's Ranger cluster under Grant No. TG-PHY990007N. Computations were also performed on the GPC supercomputer at the SciNet HPC Consortium. SciNet is funded by: the Canada Foundation for Innovation under the auspices of Compute Canada; the Government of Ontario; Ontario Research Fund\u2014Research Excellence; and the University of Toronto.\n\nPublished - Foucart2011p12691Phys_Rev_D.pdf
Submitted - 1007.4203.pdf
", "abstract": "The spin of black holes in black hole-neutron star binaries can have a strong influence on the merger dynamics and the post-merger state; a wide variety of spin magnitudes and orientations are expected to occur in nature. In this paper, we report the first simulations in full general relativity of black hole-neutron star mergers with misaligned black hole spin. We vary the spin magnitude from a_(BH)/M_(BH) = 0 to a_(BH)/M_(BH) = 0.9 for aligned cases, and we vary the misalignment angle from 0 to 80\u00b0 for a_(BH)/M_(BH) = 0.5. We restrict our study to 3:1 mass-ratio systems and use a simple \u0393-law equation of state. We find that the misalignment angle has a strong effect on the mass of the post-merger accretion disk, but only for angles greater than \u2248 40\u00b0. Although the disk mass varies significantly with spin magnitude and misalignment angle, we find that all disks have very similar lifetimes \u2248 100\u2009\u2009ms. Their thermal and rotational profiles are also very similar. For a misaligned merger, the disk is tilted with respect to the final black hole's spin axis. This will cause the disk to precess, but on a time scale longer than the accretion time. In all cases, we find promising setups for gamma-ray burst production: the disks are hot, thick, and hyperaccreting, and a baryon-clear region exists above the black hole.", "date": "2011-01-06", "date_type": "published", "publication": "Physical Review D", "volume": "83", "number": "2", "publisher": "American Physical Society", "pagerange": "Art. No. 024005", "id_number": "CaltechAUTHORS:20110301-122047796", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110301-122047796", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Sherman Fairchild Foundation" }, { "agency": "NSF", "grant_number": "PHY-0652952" }, { "agency": "NSF", "grant_number": "PHY-0652929" }, { "agency": "NSF", "grant_number": "TG-PHY990007N" }, { "agency": "NASA", "grant_number": "NNX09AF96G" } ] }, "local_group": { "items": [ { "id": "TAPIR" } ] }, "doi": "10.1103/PhysRevD.83.024005", "primary_object": { "basename": "1007.4203.pdf", "url": "https://authors.library.caltech.edu/records/cmnqz-wqt62/files/1007.4203.pdf" }, "related_objects": [ { "basename": "Foucart2011p12691Phys_Rev_D.pdf", "url": "https://authors.library.caltech.edu/records/cmnqz-wqt62/files/Foucart2011p12691Phys_Rev_D.pdf" } ], "resource_type": "article", "pub_year": "2011", "author_list": "Foucart, Francois; Duez, Matthew D.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/cfrb8-an407", "eprint_id": 86817, "eprint_status": "archive", "datestamp": "2023-08-19 04:44:51", "lastmod": "2023-10-18 20:36:48", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Mrou\u00e9-A-H", "name": { "family": "Mrou\u00e9", "given": "Abdul H." } }, { "id": "Pfeiffer-H-P", "name": { "family": "Pfeiffer", "given": "Harald P." }, "orcid": "0000-0001-9288-519X" }, { "id": "Kidder-L-E", "name": { "family": "Kidder", "given": "Lawrence E." }, "orcid": "0000-0001-5392-7342" }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Measuring orbital eccentricity and periastron advance in quasicircular black hole simulations", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2010 The American Physical Society. \n\n(Received 1 May 2010; published 8 December 2010) \n\nWe thank Geoffrey Lovelace for providing initial data for the large eccentricity run, and Luisa Buchman and Mark Scheel for providing the data for the unequal mass simulations. Results obtained in this paper were produced using the Spectral Einstein Code (SpEC) [50]. This work is supported in part by grants from the Sherman Fairchild Foundation to Caltech and Cornell, and from the Brinson Foundation to Caltech; by NSF Grant No. PHY-0601459, Grant No. PHY-0652995, and Grant No. DMS-0553302 at Caltech; by NSF Grant No. PHY-0652952, Grant No. DMS-0553677, Grant No. PHY-0652929, and NASA Grant No. NNX09AF96G at Cornell. H.\u2009P. gratefully acknowledges support from the NSERC of Canada, from the Canada Research Chairs Program, and from the Canadian Institute for Advanced Research.\n\nPublished - PhysRevD.82.124016.pdf
Submitted - 1004.4697.pdf
", "abstract": "We compare different methods of computing the orbital eccentricity of quasicircular binary black-hole systems using the orbital variables and gravitational-wave phase and frequency. For eccentricities of about a per cent, most methods work satisfactorily. For small eccentricity, however, the gravitational-wave phase allows a particularly clean and reliable measurement of the eccentricity. Furthermore, we measure the decay of the orbital eccentricity during the inspiral and find reasonable agreement with post-Newtonian results. Finally, we measure the periastron advance of nonspinning binary black holes, and we compare them to post-Newtonian approximations. With the low uncertainty in the measurement of the periastron advance, we positively detect deviations between fully numerical simulations and post-Newtonian calculations.", "date": "2010-12-15", "date_type": "published", "publication": "Physical Review D", "volume": "82", "number": "12", "publisher": "American Physical Society", "pagerange": "Art. No. 124016", "id_number": "CaltechAUTHORS:20180605-164334568", "issn": "1550-7998", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180605-164334568", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Sherman Fairchild Foundation" }, { "agency": "Brinson Foundation" }, { "agency": "NSF", "grant_number": "PHY-0601459" }, { "agency": "NSF", "grant_number": "PHY-0652995" }, { "agency": "NSF", "grant_number": "DMS-0553302" }, { "agency": "NSF", "grant_number": "PHY-0652952" }, { "agency": "NSF", "grant_number": "DMS-0553677" }, { "agency": "NSF", "grant_number": "PHY-0652929" }, { "agency": "NASA", "grant_number": "NNX09AF96G" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "Canada Research Chairs Program" }, { "agency": "Canadian Institute for Advanced Research (CIFAR)" } ] }, "local_group": { "items": [ { "id": "TAPIR" } ] }, "doi": "10.1103/PhysRevD.82.124016", "primary_object": { "basename": "1004.4697.pdf", "url": "https://authors.library.caltech.edu/records/cfrb8-an407/files/1004.4697.pdf" }, "related_objects": [ { "basename": "PhysRevD.82.124016.pdf", "url": "https://authors.library.caltech.edu/records/cfrb8-an407/files/PhysRevD.82.124016.pdf" } ], "resource_type": "article", "pub_year": "2010", "author_list": "Mrou\u00e9, Abdul H.; Pfeiffer, Harald P.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/sy9hz-w5k25", "eprint_id": 19458, "eprint_status": "archive", "datestamp": "2023-08-19 03:19:05", "lastmod": "2023-10-20 20:43:14", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Taylor-N-W", "name": { "family": "Taylor", "given": "Nicholas W." } }, { "id": "Kidder-L-E", "name": { "family": "Kidder", "given": "Lawrence E." }, "orcid": "0000-0001-5392-7342" }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Spectral methods for the wave equation in second-order form", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2010 The American Physical Society. \n\nReceived 17 May 2010; published 28 July 2010. \n\nWe would like to thank Carsten Gundlach, Jan Hesthaven, and Manuel Tiglio for valuable comments. Most of the numerical tests were performed within the framework of the Spectral Einstein Code (SpEC) developed at Cornell and Caltech primarily by L. K., Harald Pfeiffer, and Mark Scheel [23]. This work is supported in part by grants from the Sherman Fairchild Foundation to Caltech and Cornell, and from the Brinson Foundation to Caltech, by NSF Grants No. PHY-0601459, No. PHY-0652995, and No. DMS-0553302 at Caltech, by NSF Grants No. PHY-0652952, No. DMS-0553677, No. PHY-0652929, and NASA Grant No. NNX09AF96G at Cornell.\n\nPublished - Taylor2010p11028Phys_Rev_D.pdf
Submitted - 1005.2922.pdf
", "abstract": "Current spectral simulations of Einstein's equations require writing the equations in first-order form, potentially introducing instabilities and inefficiencies. We present a new penalty method for pseudospectral evolutions of second order in space wave equations. The penalties are constructed as functions of Legendre polynomials and are added to the equations of motion everywhere, not only on the boundaries. Using energy methods, we prove semidiscrete stability of the new method for the scalar wave equation in flat space and show how it can be applied to the scalar wave on a curved background. Numerical results demonstrating stability and convergence for multidomain second-order scalar wave evolutions are also presented. This work provides a foundation for treating Einstein's equations directly in second-order form by spectral methods.", "date": "2010-07-28", "date_type": "published", "publication": "Physical Review D", "volume": "82", "number": "2", "publisher": "American Physical Society", "pagerange": "Art. No. 024037", "id_number": "CaltechAUTHORS:20100817-080404692", "issn": "1550-7998", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100817-080404692", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Sherman Fairchild Foundation" }, { "agency": "Brinson Foundation" }, { "agency": "NSF", "grant_number": "PHY-0601459" }, { "agency": "NSF", "grant_number": "PHY-0652995" }, { "agency": "NSF", "grant_number": "DMS-0553302" }, { "agency": "NSF", "grant_number": "PHY-0652952" }, { "agency": "NSF", "grant_number": "DMS-0553677" }, { "agency": "NSF", "grant_number": "PHY-0652929" }, { "agency": "NASA", "grant_number": "NNX09AF96G" } ] }, "collection": "CaltechAUTHORS", "local_group": { "items": [ { "id": "TAPIR", "value": "TAPIR" } ] }, "doi": "10.1103/PhysRevD.82.024037", "primary_object": { "basename": "1005.2922.pdf", "url": "https://authors.library.caltech.edu/records/sy9hz-w5k25/files/1005.2922.pdf" }, "related_objects": [ { "basename": "Taylor2010p11028Phys_Rev_D.pdf", "url": "https://authors.library.caltech.edu/records/sy9hz-w5k25/files/Taylor2010p11028Phys_Rev_D.pdf" } ], "resource_type": "article", "pub_year": "2010", "author_list": "Taylor, Nicholas W.; Kidder, Lawrence E.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/c6g2p-sfp54", "eprint_id": 18536, "eprint_status": "archive", "datestamp": "2023-08-19 02:47:39", "lastmod": "2023-10-20 16:29:54", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Duez-M-D", "name": { "family": "Duez", "given": "Matthew D." }, "orcid": "0000-0002-0050-1783" }, { "id": "Foucart-F", "name": { "family": "Foucart", "given": "Francois" }, "orcid": "0000-0003-4617-4738" }, { "id": "Kidder-L-E", "name": { "family": "Kidder", "given": "Lawrence E." }, "orcid": "0000-0001-5392-7342" }, { "id": "Ott-C-D", "name": { "family": "Ott", "given": "Christian D." }, "orcid": "0000-0003-4993-2055" }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Equation of state effects in black hole\u2013neutron star mergers", "ispublished": "pub", "full_text_status": "public", "keywords": "Gravitation and cosmology, Astrophysics and astroparticles", "note": "\u00a9 2010 IOP Publishing Ltd. \n\nReceived 18 December 2009, in final form 19 January 2010. Published 10 May 2010. \n\nWe thank Evan O'Connor, Harald Pfeiffer and Manuel Tiglio for useful discussions. This work was supported in part by a grant from the Sherman Fairchild Foundation, by NSF grants PHY-0652952 and PHY-0652929 and NASA grant NNX09AF96G. CDO is partially supported through NSF award no AST-0855535. This research was supported in part by the NSF through TeraGrid [42] resources provided by LONI's Queen Bee and NCSA's Ranger clusters. Computations were also performed on the GPC supercomputer at the SciNet HPC Consortium. SciNet is funded by the Canada Foundation for Innovation under the auspices of Compute Canada; the Government of Ontario; Ontario Research Fund\u2013Research Excellence and the University of Toronto. We thank Harald Pfeiffer for getting us access to SciNet by compiling SpEC and submitting our runs there.\n\nPublished - Duez2010p10129Classical_Quant_Grav.pdf
Submitted - 0912.3528.pdf
", "abstract": "The merger dynamics of a black hole\u2013neutron star (BHNS) binary is influenced by the neutron star equation of state (EoS) through the latter's effect on the neutron star's radius and on the character of the mass transfer onto the black hole. We study these effects by simulating a number of BHNS binaries in full general relativity using a mixed pseudospectral/finite difference code. We consider several models of the neutron star matter EoS, including \u0393 = 2 and \u0393 = 2.75 polytropes and the nuclear-theory-based Shen EoS. For models using the Shen EoS, we consider two limits for the evolution of the composition: source-free advection and instantaneous \u03b2-equilibrium. To focus on EoS effects, we fix the mass ratio to 3:1 and the initial aligned black hole spin to a/m = 0.5 for all models. We confirm earlier studies which found that more compact stars create a stronger gravitational wave signal but a smaller postmerger accretion disk. We also vary the EoS while holding the compaction fixed. All mergers are qualitatively similar, but we find signatures of the EoS in the waveform and in the tail and disk structures.", "date": "2010-06-07", "date_type": "published", "publication": "Classical and Quantum Gravity", "volume": "27", "number": "11", "publisher": "IOP", "pagerange": "Art. No. 114106", "id_number": "CaltechAUTHORS:20100602-153604354", "issn": "0264-9381", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100602-153604354", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Sherman Fairchild Foundation" }, { "agency": "NSF", "grant_number": "PHY-0652952" }, { "agency": "NSF", "grant_number": "PHY-0652929" }, { "agency": "NASA", "grant_number": "NNX09AF96G" }, { "agency": "NSF", "grant_number": "AST-0855535" }, { "agency": "Canada Foundation for Innovation" }, { "agency": "Compute Canada" } ] }, "local_group": { "items": [ { "id": "TAPIR" } ] }, "doi": "10.1088/0264-9381/27/11/114106", "primary_object": { "basename": "0912.3528.pdf", "url": "https://authors.library.caltech.edu/records/c6g2p-sfp54/files/0912.3528.pdf" }, "related_objects": [ { "basename": "Duez2010p10129Classical_Quant_Grav.pdf", "url": "https://authors.library.caltech.edu/records/c6g2p-sfp54/files/Duez2010p10129Classical_Quant_Grav.pdf" } ], "resource_type": "article", "pub_year": "2010", "author_list": "Duez, Matthew D.; Foucart, Francois; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/qwzkc-wkz78", "eprint_id": 86820, "eprint_status": "archive", "datestamp": "2023-08-20 02:18:20", "lastmod": "2023-10-18 20:36:58", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Pazos-E", "name": { "family": "Pazos", "given": "Enrique" } }, { "id": "Tiglio-M", "name": { "family": "Tiglio", "given": "Manuel" } }, { "id": "Duez-M-D", "name": { "family": "Duez", "given": "Matthew D." }, "orcid": "0000-0002-0050-1783" }, { "id": "Kidder-L-E", "name": { "family": "Kidder", "given": "Lawrence E." }, "orcid": "0000-0001-5392-7342" }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Orbiting binary black hole evolutions with a multipatch high order finite-difference approach", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2009 The American Physical Society. \n\nReceived 6 April 2009; published 21 July 2009. \n\nThe numerical simulations presented here were performed using the Spectral Einstein Code (SpEC) developed at Caltech and Cornell primarily by L. Kidder, M. Scheel, and H. Pfeiffer. This research has been supported in part by NSF Grant No. PHY-0801213 to the University of Maryland, by NSF Grant Nos. PHY-0652952, DMS-0553677, and PHY-0652929 and by a grant from the Sherman Fairchild Foundation to Cornell, by the TeraGrid allocation TG-MCA02N014 to Louisiana State University, and by supercomputing resources at LONI. We thank O. Korobkin for his help on the early stages of this project.\n\nPublished - PhysRevD.80.024027.pdf
Submitted - 0904.0493.pdf
", "abstract": "We present numerical simulations of orbiting black holes for around 12 cycles, using a high order multipatch approach. Unlike some other approaches, the computational speed scales almost perfectly for thousands of processors. Multipatch methods are an alternative to adaptive mesh refinement, with benefits of simplicity and better scaling for improving the resolution in the wave zone. The results presented here pave the way for multipatch evolutions of black hole-neutron star and neutron star-neutron star binaries, where high resolution grids are needed to resolve details of the matter flow.", "date": "2009-07-15", "date_type": "published", "publication": "Physical Review D", "volume": "80", "number": "2", "publisher": "American Physical Society", "pagerange": "Art. No. 024027", "id_number": "CaltechAUTHORS:20180606-083847653", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180606-083847653", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY-0801213" }, { "agency": "NSF", "grant_number": "PHY-0652952" }, { "agency": "NSF", "grant_number": "DMS-0553677" }, { "agency": "NSF", "grant_number": "PHY-0652929" }, { "agency": "Sherman Fairchild Foundation" } ] }, "doi": "10.1103/PhysRevD.80.024027", "primary_object": { "basename": "0904.0493.pdf", "url": "https://authors.library.caltech.edu/records/qwzkc-wkz78/files/0904.0493.pdf" }, "related_objects": [ { "basename": "PhysRevD.80.024027.pdf", "url": "https://authors.library.caltech.edu/records/qwzkc-wkz78/files/PhysRevD.80.024027.pdf" } ], "resource_type": "article", "pub_year": "2009", "author_list": "Pazos, Enrique; Tiglio, Manuel; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/z5k62-ppb75", "eprint_id": 86828, "eprint_status": "archive", "datestamp": "2023-08-20 01:44:03", "lastmod": "2023-10-18 20:37:18", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bondarescu-R", "name": { "family": "Bondarescu", "given": "Ruxandra" } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" }, { "id": "Wasserman-I", "name": { "family": "Wasserman", "given": "Ira" } } ] }, "title": "Spinning down newborn neutron stars: Nonlinear development of the r-mode instability", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2009 American Physical Society. \n\n(Received 19 September 2008; published 1 May 2009) \n\nWe thank Sharon Morsink and Jeandrew Brink for useful discussions in understanding the effect of high spin frequencies on coupling coefficients and detuning. We are grateful to Badri Krishnan for providing us with the Advanced LIGO and Einstein Telescope noise curves from their paper [38]. We thank David Shoemaker for another Advanced LIGO noise curve. R.\u2009B. is grateful to Jayashree Balakrishna and Gregory Daues for hospitality during her stay in St. Louis for the April APS meeting, discussions, and their constant friendship and support. She also thanks Andrew Lundgren for support and useful discussions. This research was funded by NSF Grant No. AST-0606710 and No. PHY-0652952 at Cornell University. R.\u2009B. also acknowledges the support of National Science Foundation Grant No. PHY 06-53462 and No. PHY 05-55615, and NASA Grant No. NNG05GF71G, from The Pennsylvania State University.\n\nPublished - PhysRevD.79.104003.pdf
Submitted - 0809.3448
", "abstract": "We model the nonlinear saturation of the r-mode instability via three-mode couplings and the effects of the instability on the spin evolution of young neutron stars. We include one mode triplet consisting of the r-mode and two near-resonant inertial modes that couple to it. We find that the spectrum of evolutions is more diverse than previously thought. We start our evolutions with a star of temperature \u223c10^(10) K and a spin frequency close to the Kepler break-up frequency. We assume that hyperon bulk viscosity dominates at high temperatures (T\u223c10^(9)\u201310^(10) K) and boundary layer viscosity dominates at lower temperatures (\u223ca few \u00d7 10^8 K). To explore possible nonlinear behavior, we vary properties of the star such as the hyperon superfluid transition temperature, the strength of the boundary layer viscosity, and the fraction of the star that cools via direct URCA reactions. The evolution of the star is dynamic and initially dominated by fast neutrino cooling. Nonlinear effects become important when the r-mode amplitude grows above its first parametric instability threshold. The balance between neutrino cooling and viscous heating plays an important role in the evolution. Depending on the initial r-mode amplitude, and on the strength of the viscosity and of the cooling this balance can occur at different temperatures. If thermal equilibrium occurs on the r-mode stability curve, where gravitational driving equals viscous damping, the evolution may be adequately described by a one-mode model. Otherwise, nonlinear effects are important and lead to various more complicated scenarios. Once thermal balance occurs, the star spins down oscillating between thermal equilibrium states until the instability is no longer active. The average evolution of the mode amplitudes can be approximated by quasistationary states that are determined algebraically. For lower viscosity we observe runaway behavior in which the \nr-mode amplitude passes several parametric instability thresholds. In this case more modes need to be included to model the evolution accurately. In the most optimistic case, we find that gravitational radiation from the r-mode instability in a very young, fast spinning neutron star within about 1 Mpc of Earth may be detectable by advanced LIGO for years, and perhaps decades, after formation. Details regarding the amplitude and duration of the emission depend on the internal dissipation of the modes of the star, which would be probed by such detections.", "date": "2009-05-15", "date_type": "published", "publication": "Physical Review D", "volume": "79", "number": "10", "publisher": "American Physical Society", "pagerange": "Art. No. 104003", "id_number": "CaltechAUTHORS:20180606-094237094", "issn": "1550-7998", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180606-094237094", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-0606710" }, { "agency": "NSF", "grant_number": "PHY-0652952" }, { "agency": "NSF", "grant_number": "PHY 06-53462" }, { "agency": "NSF", "grant_number": "PHY 05-55615" }, { "agency": "NASA", "grant_number": "NNG05GF71G" } ] }, "doi": "10.1103/PhysRevD.79.104003", "primary_object": { "basename": "0809.3448", "url": "https://authors.library.caltech.edu/records/z5k62-ppb75/files/0809.3448" }, "related_objects": [ { "basename": "PhysRevD.79.104003.pdf", "url": "https://authors.library.caltech.edu/records/z5k62-ppb75/files/PhysRevD.79.104003.pdf" } ], "resource_type": "article", "pub_year": "2009", "author_list": "Bondarescu, Ruxandra; Teukolsky, Saul A.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/1hd53-63f09", "eprint_id": 86864, "eprint_status": "archive", "datestamp": "2023-08-20 01:05:01", "lastmod": "2023-10-18 20:39:25", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Gottfried-K", "name": { "family": "Gottfried", "given": "Kurt" } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul" }, "orcid": "0000-0001-9765-4526" }, { "id": "Wasserman-I", "name": { "family": "Wasserman", "given": "Ira" } } ] }, "title": "Edwin Ernest Salpeter", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2009 AIP Publishing.\n\nPublished - 1.3099585.pdf
", "abstract": "Edwin Ernest Salpeter, among the most influential, prescient, and innovative astrophysicists of the past half century, died of leukemia at his home in Ithaca, New York, on 26 November 2008.", "date": "2009-03", "date_type": "published", "publication": "Physics Today", "volume": "62", "number": "3", "publisher": "American Institute of Physics", "pagerange": "65", "id_number": "CaltechAUTHORS:20180606-155643335", "issn": "0031-9228", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180606-155643335", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "doi": "10.1063/1.3099585", "primary_object": { "basename": "1.3099585.pdf", "url": "https://authors.library.caltech.edu/records/1hd53-63f09/files/1.3099585.pdf" }, "resource_type": "article", "pub_year": "2009", "author_list": "Gottfried, Kurt; Teukolsky, Saul; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/24hk6-wgr13", "eprint_id": 86855, "eprint_status": "archive", "datestamp": "2023-08-20 00:43:00", "lastmod": "2023-10-18 20:38:48", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" }, { "id": "Wasserman-I", "name": { "family": "Wasserman", "given": "Ira" } } ] }, "title": "Obituary: Edwin Salpeter (1924\u20132008)", "ispublished": "pub", "full_text_status": "restricted", "note": "\u00a9 2009 Macmillan Publishers Limited.", "abstract": "Edwin Ernest Salpeter, who perhaps more than anyone put the physics into astrophysics, died on 26 November 2008 at the age of 83. Among his many accomplishments was figuring out how giant stars burn helium to form carbon in the 'triple-alpha process' (named after the three helium nuclei \u2014 alpha particles \u2014 that fuse together in the process). Before this discovery, the origin of the elements beyond helium in the periodic table was a mystery.", "date": "2009-01-15", "date_type": "published", "publication": "Nature", "volume": "457", "number": "7227", "publisher": "Nature Publishing Group", "pagerange": "275", "id_number": "CaltechAUTHORS:20180606-145913301", "issn": "0028-0836", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180606-145913301", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "doi": "10.1038/457275a", "resource_type": "article", "pub_year": "2009", "author_list": "Teukolsky, Saul A. and Wasserman, Ira" }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/2m2y3-21r42", "eprint_id": 12389, "eprint_status": "archive", "datestamp": "2023-08-22 13:36:02", "lastmod": "2023-10-17 16:43:35", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Duez-M-D", "name": { "family": "Duez", "given": "Matthew D." }, "orcid": "0000-0002-0050-1783" }, { "id": "Foucart-F", "name": { "family": "Foucart", "given": "Francois" }, "orcid": "0000-0003-4617-4738" }, { "id": "Kidder-L-E", "name": { "family": "Kidder", "given": "Lawrence E." }, "orcid": "0000-0001-5392-7342" }, { "id": "Pfeiffer-H-P", "name": { "family": "Pfeiffer", "given": "Harald P." }, "orcid": "0000-0001-9288-519X" }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Evolving black hole-neutron star binaries in general relativity using pseudospectral and finite difference methods", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2008 The American Physical Society. \n\n(Received 29 August 2008; published 13 November 2008) \n\nWe thank Francois Limousin and Manuel Tiglio for useful discussions. This work was supported in part by grants from the Sherman Fairchild Foundation to Caltech and Cornell and from the Brinson Foundation to Caltech; by NSF Grants No. PHY-0601459, No. PHY-0652995, No. DMS-0553302 and NASA Grant No. NNG05GG52G at Caltech; by NSF Grants No. PHY-0652952, No. DMS-0553677, No. PHY-0652929, and NASA Grant No. NNG05GG51G at Cornell. This research was supported in part by the NSF through TeraGrid [75] resources provided by LONI's Queen Bee cluster. Computations were also performed on Caltech's Shared Heterogeneous Cluster (SHC).\n\nPublished - DUEprd08.pdf
Submitted - 0809.0002.pdf
", "abstract": "We present a code for solving the coupled Einstein-hydrodynamics equations to evolve relativistic, self-gravitating fluids. The Einstein field equations are solved in generalized harmonic coordinates on one grid using pseudospectral methods, while the fluids are evolved on another grid using shock-capturing finite difference or finite volume techniques. We show that the code accurately evolves equilibrium stars and accretion flows. Then we simulate an equal-mass nonspinning black hole-neutron star binary, evolving through the final four orbits of inspiral, through the merger, to the final stationary black hole. The gravitational waveform can be reliably extracted from the simulation.", "date": "2008-11-15", "date_type": "published", "publication": "Physical Review D", "volume": "78", "number": "10", "publisher": "American Physical Society", "pagerange": "Art. No. 104015", "id_number": "CaltechAUTHORS:DUEprd08", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:DUEprd08", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Sherman Fairchild Foundation" }, { "agency": "Brinson Foundation" }, { "agency": "NSF", "grant_number": "PHY-0601459" }, { "agency": "NSF", "grant_number": "PHY-0652995" }, { "agency": "NSF", "grant_number": "DMS-0553302" }, { "agency": "NASA", "grant_number": "NNG05GG52G" }, { "agency": "NSF", "grant_number": "PHY-0652952" }, { "agency": "NSF", "grant_number": "DMS-0553677" }, { "agency": "NSF", "grant_number": "PHY-0652929" }, { "agency": "NASA", "grant_number": "NNG05GG51G" } ] }, "local_group": { "items": [ { "id": "TAPIR" } ] }, "doi": "10.1103/PhysRevD.78.104015", "primary_object": { "basename": "0809.0002.pdf", "url": "https://authors.library.caltech.edu/records/2m2y3-21r42/files/0809.0002.pdf" }, "related_objects": [ { "basename": "DUEprd08.pdf", "url": "https://authors.library.caltech.edu/records/2m2y3-21r42/files/DUEprd08.pdf" } ], "resource_type": "article", "pub_year": "2008", "author_list": "Duez, Matthew D.; Foucart, Francois; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/4qkw2-ndx15", "eprint_id": 86821, "eprint_status": "archive", "datestamp": "2023-08-19 23:29:31", "lastmod": "2023-10-18 20:37:01", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Mrou\u00e9-A-H", "name": { "family": "Mrou\u00e9", "given": "Abdul H." } }, { "id": "Kidder-L-E", "name": { "family": "Kidder", "given": "Lawrence E." }, "orcid": "0000-0001-5392-7342" }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Ineffectiveness of Pad\u00e9 resummation techniques in post-Newtonian approximations", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2008 The American Physical Society. \n\nReceived 15 May 2008; published 4 August 2008. \n\nIt is a pleasure to acknowledge useful discussions with Emanuele Berti, Michael Boyle, Alessandra Buonanno, Lee Lindblom, Harald P. Pfeiffer, Yi Pan, Mark A. Scheel, and Nicol\u00e1s Yunes. We thank Jihad Touma for helpful discussions about Pad\u00e9 approximants, Harald P. Pfeiffer and Michael Boyle for providing the numerical data of the flux in the equal mass case, and Eric Poisson for providing the numerical data of the flux in the test mass limit. This work was supported in part by grants from the Sherman Fairchild Foundation to Cornell; by NSF Grant Nos. PHY-0652952, DMS-0553677, PHY-0652929, and NASA Grant No. NNG05GG51G at Cornell.\n\nPublished - PhysRevD.78.044004.pdf
Submitted - 0805.2390.pdf
", "abstract": "We test the resummation techniques used in developing Pad\u00e9 and effective one body (EOB) waveforms for gravitational wave detection. Convergence tests show that Pad\u00e9 approximants of the gravitational wave energy flux do not accelerate the convergence of the standard Taylor approximants even in the test mass limit, and there is no reason why Pad\u00e9 transformations should help in estimating parameters better in data analysis. Moreover, adding a pole to the flux seems unnecessary in the construction of these Pad\u00e9-approximated flux formulas. Pad\u00e9 approximants may be useful in suggesting the form of fitting formulas. We compare a 15-orbit numerical waveform of the Caltech-Cornell group to the suggested Pad\u00e9 waveforms of Damour et al. in the equal mass, nonspinning quasicircular case. The comparison suggests that the Pad\u00e9 waveforms do not agree better with the numerical waveform than the standard Taylor based waveforms. Based on this result, we design a simple EOB model by modifiying the Taylor-expanded EOB model of Buonanno et al., using the Taylor series of the flux with an unknown parameter at the fourth post-Newtonian order that we fit for. The 4PN parameter incorporates higher order effects of the radiation reaction. This simple EOB model generates a waveform having a phase difference of only 0.002 radians with the numerical waveform, much smaller than 0.04 radians the phase uncertainty in the numerical data itself. An EOB Hamiltonian can make use of a Pad\u00e9 transformation in its construction, but this is the only place Pad\u00e9 transformations seem useful.", "date": "2008-08-15", "date_type": "published", "publication": "Physical Review D", "volume": "78", "number": "4", "publisher": "American Physical Society", "pagerange": "Art. No. 044004", "id_number": "CaltechAUTHORS:20180606-084613563", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180606-084613563", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Sherman Fairchild Foundation" }, { "agency": "NSF", "grant_number": "PHY-0652952" }, { "agency": "NSF", "grant_number": "DMS-0553677" }, { "agency": "NSF", "grant_number": "PHY-0652929" }, { "agency": "NASA", "grant_number": "NNG05GG51G" } ] }, "doi": "10.1103/PhysRevD.78.044004", "primary_object": { "basename": "0805.2390.pdf", "url": "https://authors.library.caltech.edu/records/4qkw2-ndx15/files/0805.2390.pdf" }, "related_objects": [ { "basename": "PhysRevD.78.044004.pdf", "url": "https://authors.library.caltech.edu/records/4qkw2-ndx15/files/PhysRevD.78.044004.pdf" } ], "resource_type": "article", "pub_year": "2008", "author_list": "Mrou\u00e9, Abdul H.; Kidder, Lawrence E.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/q4hwq-0wr93", "eprint_id": 11113, "eprint_status": "archive", "datestamp": "2023-08-22 12:00:18", "lastmod": "2023-10-16 23:17:29", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Foucart-F", "name": { "family": "Foucart", "given": "Francois" }, "orcid": "0000-0003-4617-4738" }, { "id": "Kidder-L-E", "name": { "family": "Kidder", "given": "Lawrence E." }, "orcid": "0000-0001-5392-7342" }, { "id": "Pfeiffer-H-P", "name": { "family": "Pfeiffer", "given": "Harald P." }, "orcid": "0000-0001-9288-519X" }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Initial data for black hole\u2013neutron star binaries: A flexible, high-accuracy spectral method", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2008 The American Physical Society. \n\n(Received 24 April 2008; published 27 June 2008) \n\nIt is a pleasure to acknowledge useful discussions with Matthew Duez, Eanna Flanagan, Jan Hesthaven, Francois Limousin, Geoffrey Lovelace, Robert Owen, Mark Scheel, and Manuel Tiglio. In particular, we would like to thank Matthew Duez for his help in evolving low-eccentricity binaries, Jan Hesthaven for his contribution to the improvement of the preconditioner in SPELLS, Geoffrey Lovelace for his advice on the construction of spinning black holes, and Robert Owen for the measurement of these spins. This work was supported in part by grants from the Sherman Fairchild Foundation to Caltech and Cornell, and from the Brinson Foundation to Caltech; by NSF Grants No. PHY-0652952, No. DMS-0553677, and No. PHY-0652929, and NASA Grant No. NNG05GG51G at Cornell; and by NSF Grants No. PHY-0601459, No. PHY-0652995 and NASA Grant No. NNG05GG52G at Caltech.\n\nPublished - FOUprd08.pdf
Submitted - 0804.3787.pdf
", "abstract": "We present a new numerical scheme to solve the initial value problem for black hole\u2013neutron star binaries. This method takes advantage of the flexibility and fast convergence of a multidomain spectral representation of the initial data to construct high-accuracy solutions at a relatively low computational cost. We provide convergence tests of the method for both isolated neutron stars and irrotational binaries. In the second case, we show that we can resolve the small inconsistencies that are part of the quasiequilibrium formulation, and that these inconsistencies are significantly smaller than observed in previous works. The possibility of generating a wide variety of initial data is also demonstrated through two new configurations inspired by results from binary black holes. First, we show that choosing a modified Kerr-Schild conformal metric instead of a flat conformal metric allows for the construction of quasiequilibrium binaries with a spinning black hole. Second, we construct binaries in low-eccentricity orbits, which are a better approximation to astrophysical binaries than quasiequilibrium systems.", "date": "2008-06-15", "date_type": "published", "publication": "Physical Review D", "volume": "77", "number": "12", "publisher": "American Physical Society", "pagerange": "Art. No. 124051", "id_number": "CaltechAUTHORS:FOUprd08", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:FOUprd08", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Sherman Fairchild Foundation" }, { "agency": "Brinson Foundation" }, { "agency": "NSF", "grant_number": "PHY-0652952" }, { "agency": "NSF", "grant_number": "DMS-0553677" }, { "agency": "NSF", "grant_number": "PHY-0652929" }, { "agency": "NASA", "grant_number": "NNG05GG51G" }, { "agency": "NSF", "grant_number": "PHY-0601459" }, { "agency": "NSF", "grant_number": "PHY-0652995" }, { "agency": "NASA", "grant_number": "NNG05GG52G" } ] }, "doi": "10.1103/PhysRevD.77.124051", "primary_object": { "basename": "FOUprd08.pdf", "url": "https://authors.library.caltech.edu/records/q4hwq-0wr93/files/FOUprd08.pdf" }, "related_objects": [ { "basename": "0804.3787.pdf", "url": "https://authors.library.caltech.edu/records/q4hwq-0wr93/files/0804.3787.pdf" } ], "resource_type": "article", "pub_year": "2008", "author_list": "Foucart, Francois; Kidder, Lawrence E.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/dpzg4-3ma04", "eprint_id": 86849, "eprint_status": "archive", "datestamp": "2023-08-19 22:44:50", "lastmod": "2023-10-18 20:38:34", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Tiglio-M", "name": { "family": "Tiglio", "given": "Manuel" } }, { "id": "Kidder-L-E", "name": { "family": "Kidder", "given": "Lawrence E." }, "orcid": "0000-0001-5392-7342" }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "High accuracy simulations of Kerr tails: coordinate dependence and higher multipoles", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2018 IOP Publishing. \n\nReceived 19 December 2007, in final form 31 March 2008. Published 7 May 2008. \n\nThis research was supported in part by NSF grant PHY 0505761 to Louisiana State University, by a grant from the Sherman Fairchild Foundation to Cornell, and by NSF grants PHY-0652952, DMS-0553677, PHY-0652929 and NASA grant NNG05GG51G at Cornell. The research employed the resources of the CCT at LSU, which is supported by funding from the Louisiana legislature's Information Technology Initiative. MT would like to thank Enrique Pazos and Jorge Pullin for helpful discussions throughout this project and hospitality at Cornell University, where this work was done.\n\nSubmitted - 0712.2472.pdf
", "abstract": "We investigate the late-time behavior of a scalar field on a fixed Kerr background using a 2 + 1 dimensional pseudo-spectral evolution code. We compare evolutions of pure axisymmetric multipoles in both Kerr\u2013Schild and Boyer\u2013Lindquist coordinates. We find that the late-time power-law decay rate depends upon the slicing of the background, confirming previous theoretical predictions for those decay rates. The accuracy of the numerical evolutions is sufficient to decide unambiguously between competing claims in the literature.", "date": "2008-05-21", "date_type": "published", "publication": "Classical and Quantum Gravity", "volume": "25", "number": "10", "publisher": "IOP", "pagerange": "Art. No. 105022", "id_number": "CaltechAUTHORS:20180606-131328537", "issn": "0264-9381", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180606-131328537", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY-0505761" }, { "agency": "Sherman Fairchild Foundation" }, { "agency": "NSF", "grant_number": "PHY-0652952" }, { "agency": "NSF", "grant_number": "DMS-0553677" }, { "agency": "NSF", "grant_number": "PHY-0652929" }, { "agency": "NASA", "grant_number": "NNG05GG51G" } ] }, "doi": "10.1088/0264-9381/25/10/105022", "primary_object": { "basename": "0712.2472.pdf", "url": "https://authors.library.caltech.edu/records/dpzg4-3ma04/files/0712.2472.pdf" }, "resource_type": "article", "pub_year": "2008", "author_list": "Tiglio, Manuel; Kidder, Lawrence E.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/apwg4-rjz09", "eprint_id": 9422, "eprint_status": "archive", "datestamp": "2023-08-22 10:43:22", "lastmod": "2023-10-16 22:12:18", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Boyle-M", "name": { "family": "Boyle", "given": "Michael" } }, { "id": "Brown-D-A", "name": { "family": "Brown", "given": "Duncan A." }, "orcid": "0000-0002-9180-5765" }, { "id": "Kidder-L-E", "name": { "family": "Kidder", "given": "Lawrence E." }, "orcid": "0000-0001-5392-7342" }, { "id": "Mrou\u00e9-A-H", "name": { "family": "Mrou\u00e9", "given": "Abdul H." } }, { "id": "Pfeiffer-H-P", "name": { "family": "Pfeiffer", "given": "Harald P." }, "orcid": "0000-0001-9288-519X" }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." } }, { "id": "Cook-G-B", "name": { "family": "Cook", "given": "Gregory B." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "High-accuracy comparison of numerical relativity simulations with post-Newtonian expansions", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2007 The American Physical Society. \n\n(Received 30 September 2007; published 27 December 2007) \n\nIt is a pleasure to acknowledge useful discussions with Stuart Anderson, Alessandra Buonanno, Mark Hannam, Ian Hinder, Luis Lehner, Lee Lindblom, Geoffrey Lovelace, Sean McWilliams, Robert Owen, Yi Pan, Oliver Rinne, and Kip Thorne. In particular, we would like to thank Alessandra Buonanno for a careful reading of this manuscript, Rob Owen for estimating the BH spin, Geoffrey Lovelace for his help constructing initial data, Oliver Rinne for providing improved boundary conditions, and Lee Lindblom for his guidance and input throughout this project. This work was supported in part by grants from the Sherman Fairchild Foundation to Caltech and Cornell, and from the Brinson Foundation to Caltech; by NSF Grants No. PHY-0601459, No. PHY-0652995, No. DMS-0553302 and NASA Grant No. NNG05GG52G at Caltech; by NSF Grants No. PHY-0652952, No. DMS-0553677, No. PHY-0652929 and NASA Grant No. NNG05GG51G at Cornell; and by the Z. Smith Reynolds Foundation and NSF Grant No. PHY-0555617 at Wake Forest. We thank NASA/JPL for providing computing facilities that contributed to this work. Some of the simulations discussed here were produced with LIGO Laboratory computing facilities. LIGO was constructed by the California Institute of Technology and Massachusetts Institute of Technology with funding from the National Science Foundation and operates under cooperative agreement No. PHY-0107417. This paper has been assigned LIGO document No. LIGO-P070101-00-Z.\n\nPublished - BOYprd07b.pdf
Submitted - 0710.0158.pdf
", "abstract": "Numerical simulations of 15 orbits of an equal-mass binary black-hole system are presented. Gravitational waveforms from these simulations, covering more than 30 cycles and ending about 1.5 cycles before merger, are compared with those from quasicircular zero-spin post-Newtonian (PN) formulae. The cumulative phase uncertainty of these comparisons is about 0.05 radians, dominated by effects arising from the small residual spins of the black holes and the small residual orbital eccentricity in the simulations. Matching numerical results to PN waveforms early in the run yields excellent agreement (within 0.05 radians) over the first ~15 cycles, thus validating the numerical simulation and establishing a regime where PN theory is accurate. In the last 15 cycles to merger, however, generic time-domain Taylor approximants build up phase differences of several radians. But, apparently by coincidence, one specific post-Newtonian approximant, TaylorT4 at 3.5PN order, agrees much better with the numerical simulations, with accumulated phase differences of less than 0.05 radians over the 30-cycle waveform. Gravitational-wave amplitude comparisons are also done between numerical simulations and post-Newtonian, and the agreement depends on the post-Newtonian order of the amplitude expansion: the amplitude difference is about 6%\u20137% for zeroth order and becomes smaller for increasing order. A newly derived 3.0PN amplitude correction improves agreement significantly (<1% amplitude difference throughout most of the run, increasing to 4% near merger) over the previously known 2.5PN amplitude terms.", "date": "2007-12-15", "date_type": "published", "publication": "Physical Review D", "volume": "76", "number": "12", "publisher": "American Physical Society", "pagerange": "Art. No. 124038", "id_number": "CaltechAUTHORS:BOYprd07b", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:BOYprd07b", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Sherman Fairchild Foundation" }, { "agency": "Brinson Foundation" }, { "agency": "NSF", "grant_number": "PHY-0601459" }, { "agency": "NSF", "grant_number": "PHY-0652995" }, { "agency": "NSF", "grant_number": "DMS-0553302" }, { "agency": "NASA", "grant_number": "NNG05GG52G" }, { "agency": "NSF", "grant_number": "PHY-0652952" }, { "agency": "NSF", "grant_number": "DMS-0553677" }, { "agency": "NSF", "grant_number": "PHY-0652929" }, { "agency": "NASA", "grant_number": "NNG05GG51G" }, { "agency": "Z. Smith Reynolds Foundation" }, { "agency": "NSF", "grant_number": "PHY-0555617" }, { "agency": "NSF", "grant_number": "PHY-0107417" } ] }, "other_numbering_system": { "items": [ { "id": "P070101-00-Z", "name": "LIGO Document" } ] }, "local_group": { "items": [ { "id": "LIGO" }, { "id": "TAPIR" } ] }, "doi": "10.1103/PhysRevD.76.124038", "primary_object": { "basename": "0710.0158.pdf", "url": "https://authors.library.caltech.edu/records/apwg4-rjz09/files/0710.0158.pdf" }, "related_objects": [ { "basename": "BOYprd07b.pdf", "url": "https://authors.library.caltech.edu/records/apwg4-rjz09/files/BOYprd07b.pdf" } ], "resource_type": "article", "pub_year": "2007", "author_list": "Boyle, Michael; Brown, Duncan A.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/0c434-stt38", "eprint_id": 86822, "eprint_status": "archive", "datestamp": "2023-08-19 20:58:29", "lastmod": "2023-10-18 20:37:04", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bondarescu-R", "name": { "family": "Bondarescu", "given": "Ruxandra" } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" }, { "id": "Wasserman-I", "name": { "family": "Wasserman", "given": "Ira" } } ] }, "title": "Spin evolution of accreting neutron stars: Nonlinear development of the r-mode instability", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2007 The American Physical Society. \n\nReceived 5 April 2007; published 20 September 2007. \n\nIt is a pleasure to thank Jeandrew Brink and \u00c9anna Flanagan for useful discussions. R.\u2009B. would especially like to thank Jeandrew for useful discussions, encouragement, and advice at the beginning of this project, without which the project would not have been started. R.\u2009B. is very grateful to Gregory Daues for steady encouragement and support for the duration of this project, and also to Gabrielle Allen and Ed Seidel. This research was funded by Grants No. NSF AST-0307273, NSF AST-0606710, and NSF PHY-0354631.\n\nPublished - PhysRevD.76.064019.pdf
Submitted - 0704.0799.pdf
", "abstract": "The nonlinear saturation of the r-mode instability and its effects on the spin evolution of low mass x-ray binaries (LMXBs) are modeled using the triplet of modes at the lowest parametric instability threshold. We solve numerically the coupled equations for the three modes in conjunction with the spin and temperature evolution equations. We observe that very quickly the mode amplitudes settle into quasistationary states that change slowly as the temperature and spin of the star evolve. Once these states are reached, the mode amplitudes can be found algebraically and the system of equations is reduced from eight to two equations: spin and temperature evolution. The evolution of the neutron star angular velocity and temperature follow easily calculated trajectories along these sequences of quasistationary states. The outcome depends on whether or not the star will reach thermal equilibrium, where the viscous heating by the three modes is equal to the neutrino cooling (H=C curve). If, when the r-mode becomes unstable, the star spins at a frequency below the maximum of the H=C curve, then it will reach a state of thermal equilibrium. It can then either (1) undergo a cyclic evolution with a small cycle size with a frequency change of at most 10%, (2) evolve toward a full equilibrium state in which the accretion torque balances the gravitational radiation emission, or (3) enter a thermogravitational runaway on a very long time scale of \u224810^6\u2009\u2009years. If the star does not reach a state of thermal equilibrium, then a faster thermal runaway (time scale of \u2248100\u2009\u2009years) occurs and the r-mode amplitude increases above the second parametric instability threshold. Following this evolution requires more inertial modes to be included. The sources of damping considered are shear viscosity, hyperon bulk viscosity, and viscosity within the core-crust boundary layer. We vary proprieties of the star such as the hyperon superfluid transition temperature T_c, the fraction of the star that is above the threshold for direct URCA reactions, and slippage factor, and map the different scenarios we obtain to ranges of these parameters. We focus on Tc \u2273 5\u00d710^9\u2009\u2009K where nonlinear effects are important. Wagoner [R. Wagoner, Astrophys. J. 578, L63 (2002).] has shown that a very low r-mode amplitude arises at smaller Tc. For all our bounded evolutions the r-mode amplitude remains small \u223c10^(\u22125). The spin frequency of accreting neutron stars is limited by boundary layer viscosity to \u03bd_(max)\u2248800\u2009\u2009Hz[Sns/(M_(1.4)R_6)]^(4/11)T^(\u22122/11)_8. Fast rotators are allowed for [S_(ns)/(M_(1.4)R_6)]^(4/11)T^(\u22122/11)_8 \u223c1 and we find that in this case the r-mode instability would be active for about 1 in 1000 LMXBs and that only the gravitational waves from LMXBs in the local group of galaxies could be detected by advanced LIGO interferometers.", "date": "2007-09-15", "date_type": "published", "publication": "Physical Review D", "volume": "76", "number": "6", "publisher": "American Physical Society", "pagerange": "Art. No. 064019", "id_number": "CaltechAUTHORS:20180606-085231873", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180606-085231873", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-0307273" }, { "agency": "NSF", "grant_number": "AST-0606710" }, { "agency": "NSF", "grant_number": "PHY-0354631" } ] }, "doi": "10.1103/PhysRevD.76.064019", "primary_object": { "basename": "0704.0799.pdf", "url": "https://authors.library.caltech.edu/records/0c434-stt38/files/0704.0799.pdf" }, "related_objects": [ { "basename": "PhysRevD.76.064019.pdf", "url": "https://authors.library.caltech.edu/records/0c434-stt38/files/PhysRevD.76.064019.pdf" } ], "resource_type": "article", "pub_year": "2007", "author_list": "Bondarescu, Ruxandra; Teukolsky, Saul A.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/a7s4e-g5h65", "eprint_id": 6385, "eprint_status": "archive", "datestamp": "2023-08-22 07:14:08", "lastmod": "2023-10-16 20:18:18", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." } }, { "id": "Pfeiffer-H-P", "name": { "family": "Pfeiffer", "given": "Harald P." }, "orcid": "0000-0001-9288-519X" }, { "id": "Lindblom-L", "name": { "family": "Lindblom", "given": "Lee" } }, { "id": "Kidder-L-E", "name": { "family": "Kidder", "given": "Lawrence E." }, "orcid": "0000-0001-5392-7342" }, { "id": "Rinne-O", "name": { "family": "Rinne", "given": "Oliver" } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Solving Einstein's equations with dual coordinate frames", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2006 The American Physical Society. \n\n(Received 13 July 2006; published 2 November 2006) \n\nThis work was supported in part by a grant from the Sherman Fairchild Foundation to Caltech and Cornell, by NSF Grants No. PHY-0099568, No. PHY-0244906, and No. PHY-0601459, and NASA Grants No. NAG5-12834, No. NNG05GG52G at Caltech, and by NSF Grants No. PHY-0312072, No. PHY-0354631, and NASA Grant No. NNG05GG51G at Cornell.\n\nPublished - SCHEprd06.pdf
Submitted - 0607056.pdf
", "abstract": "A method is introduced for solving Einstein's equations using two distinct coordinate systems. The coordinate basis vectors associated with one system are used to project out components of the metric and other fields, in analogy with the way fields are projected onto an orthonormal tetrad basis. These field components are then determined as functions of a second independent coordinate system. The transformation to the second coordinate system can be thought of as a mapping from the original inertial coordinate system to the computational domain. This dual-coordinate method is used to perform stable numerical evolutions of a black-hole spacetime using the generalized harmonic form of Einstein's equations in coordinates that rotate with respect to the inertial frame at infinity; such evolutions are found to be generically unstable using a single rotating-coordinate frame. The dual-coordinate method is also used here to evolve binary black-hole spacetimes for several orbits. The great flexibility of this method allows comoving coordinates to be adjusted with a feedback control system that keeps the excision boundaries of the holes within their respective apparent horizons.", "date": "2006-11-15", "date_type": "published", "publication": "Physical Review D", "volume": "74", "number": "10", "publisher": "American Physical Society", "pagerange": "Art. No. 104006", "id_number": "CaltechAUTHORS:SCHEprd06", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:SCHEprd06", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Sherman Fairchild Foundation" }, { "agency": "NSF", "grant_number": "PHY-0099568" }, { "agency": "NSF", "grant_number": "PHY-0244906" }, { "agency": "NSF", "grant_number": "PHY-0601459" }, { "agency": "NASA", "grant_number": "NAG5-12834" }, { "agency": "NASA", "grant_number": "NNG05GG52G" }, { "agency": "NSF", "grant_number": "PHY-0312072" }, { "agency": "NSF", "grant_number": "PHY-0354631" }, { "agency": "NASA", "grant_number": "NNG05GG51G" } ] }, "local_group": { "items": [ { "id": "TAPIR" } ] }, "doi": "10.1103/PhysRevD.74.104006", "primary_object": { "basename": "0607056.pdf", "url": "https://authors.library.caltech.edu/records/a7s4e-g5h65/files/0607056.pdf" }, "related_objects": [ { "basename": "SCHEprd06.pdf", "url": "https://authors.library.caltech.edu/records/a7s4e-g5h65/files/SCHEprd06.pdf" } ], "resource_type": "article", "pub_year": "2006", "author_list": "Scheel, Mark A.; Pfeiffer, Harald P.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/hqgfh-h8163", "eprint_id": 24750, "eprint_status": "archive", "datestamp": "2023-08-22 06:23:14", "lastmod": "2024-01-13 05:18:58", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Shoemaker-D", "name": { "family": "Shoemaker", "given": "Deirdre" } }, { "id": "Pfeiffer-H", "name": { "family": "Pfeiffer", "given": "Harald" } }, { "id": "Kidder-L", "name": { "family": "Kidder", "given": "Larry" } }, { "id": "Laguna-P", "name": { "family": "Laguna", "given": "Pablo" } }, { "id": "Lindblom-L", "name": { "family": "Lindblom", "given": "Lee" } }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul" }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Mining for Observables: A New Challenge in Numerical Relativity", "ispublished": "unpub", "full_text_status": "public", "keywords": "numerical relativity; black holes; gravitational waves", "note": "\u00a9 2006 American Institute of Physics. \n\nIssue Date: 25 August 2006. \n\nThis work was supported by NSF grants PHY-9800973 and PHY-0114375, and PHY-0354821. Work supported in part by the Center for Gravitational Wave Physics funded by the National Science Foundation under Cooperative Agreement PHY-0114375.\n\nPublished - SHOaipcp06.pdf
", "abstract": "One of the motivations behind numerical relativity is to provide gravitational wave signals of compact objects to observers using the new gravitational wave detectors. Yet, because of the complexities involved, no dependable signals of binary-black hole coalescences have been established. The work in this proceedings is motivated by how numerical relativity can be used today to predict robust features in gravitational wave signals of binary black-hole coalescence by making approximations to the full problem. To illustrate this, we present results from evolving a Klein-Gordon equation on a frozen background. The background is set by a sequence of initial data in which the binary is in quasi-equilibrium. We probe the data resulting from the evolution for the transition between the linear and non-linear regimes using oscillations of the black holes as our guide. This information is used to motivate a qualitative picture of the gravitational signal of a black-hole coalescence.", "date": "2006-08-25", "date_type": "published", "publisher": "American Institute of Physics", "place_of_pub": "Melville, NY", "pagerange": "669-676", "id_number": "CaltechAUTHORS:20110808-145749171", "isbn": "0-7354-0343-0", "book_title": "Recent Advances in Astronomy and Astrophysics", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110808-145749171", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY-9800973" }, { "agency": "NSF", "grant_number": "PHY-0114375" }, { "agency": "NSF", "grant_number": "PHY-0354821" }, { "agency": "NSF", "grant_number": "PHY-0114375" } ] }, "local_group": { "items": [ { "id": "TAPIR" } ] }, "contributors": { "items": [ { "id": "Solomos-N-H", "name": { "family": "Solomos", "given": "Nikolaos H." } } ] }, "doi": "10.1063/1.2348045", "primary_object": { "basename": "SHOaipcp06.pdf", "url": "https://authors.library.caltech.edu/records/hqgfh-h8163/files/SHOaipcp06.pdf" }, "resource_type": "book_section", "pub_year": "2006", "author_list": "Shoemaker, Deirdre; Pfeiffer, Harald; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/mk1h7-64h70", "eprint_id": 86823, "eprint_status": "archive", "datestamp": "2023-08-19 15:31:00", "lastmod": "2023-10-18 20:37:06", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Brink-J", "name": { "family": "Brink", "given": "Jeandrew" } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" }, { "id": "Wasserman-I", "name": { "family": "Wasserman", "given": "Ira" } } ] }, "title": "Nonlinear coupling network to simulate the development of the r mode instability in neutron stars. II. Dynamics", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2005 The American Physical Society. \n\nReceived 25 October 2004; published 31 March 2005. \n\nThanks to Larry Kidder for helping with parallelization of the code and numerous other technical details. This research is supported in part by NSF Grant No. AST-0307273, No. PHY-9900672, and No. PHY-0312072 at Cornell University.\n\nPublished - PhysRevD.71.064029.pdf
Submitted - 0410072.pdf
", "abstract": "Two mechanisms for nonlinear mode saturation of the r mode in neutron stars have been suggested: the parametric instability mechanism involving a small number of modes and the formation of a nearly continuous Kolmogorov-type cascade. Using a network of oscillators constructed from the eigenmodes of a perfect fluid incompressible star, we investigate the transition between the two regimes numerically. Our network includes the 4995 inertial modes up to n \u2264 30 with 146\u2009998 direct couplings to the r mode and 1\u2009306\u2009999 couplings with detuning <0.002 (out of a total of approximately 10^9 possible couplings). The lowest parametric instability thresholds for a range of temperatures are calculated and it is found that the r mode becomes unstable to modes with 13 < n <15. In the undriven, undamped, Hamiltonian version of the network the rate to achieve equipartition is found to be amplitude dependent, reminiscent of the Fermi-Pasta-Ulam problem. More realistic models driven unstable by gravitational radiation and damped by shear viscosity are explored next. A range of damping rates, corresponding to temperatures 10^6\u2009\u2009K to 10^9\u2009\u2009K, is considered. Exponential growth of the r mode is found to cease at small amplitudes \u224810^(\u22124). For strongly damped, low temperature models, a few modes dominate the dynamics. The behavior of the r mode is complicated, but its amplitude is still no larger than about 10^(\u22124) on average. For high temperature, weakly damped models the r mode feeds energy into a sea of oscillators that achieve approximate equipartition. In this case the r-mode amplitude settles to a value for which the rate to achieve equipartition is approximately the linear instability growth rate.", "date": "2005-03-15", "date_type": "published", "publication": "Physical Review D", "volume": "71", "number": "6", "publisher": "American Physical Society", "pagerange": "Art. No. 064029", "id_number": "CaltechAUTHORS:20180606-090026723", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180606-090026723", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-0307273" }, { "agency": "NSF", "grant_number": "PHY-9900672" }, { "agency": "NSF", "grant_number": "PHY-0312072" } ] }, "doi": "10.1103/PhysRevD.71.064029", "primary_object": { "basename": "0410072.pdf", "url": "https://authors.library.caltech.edu/records/mk1h7-64h70/files/0410072.pdf" }, "related_objects": [ { "basename": "PhysRevD.71.064029.pdf", "url": "https://authors.library.caltech.edu/records/mk1h7-64h70/files/PhysRevD.71.064029.pdf" } ], "resource_type": "article", "pub_year": "2005", "author_list": "Brink, Jeandrew; Teukolsky, Saul A.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/ddkdw-tk513", "eprint_id": 86819, "eprint_status": "archive", "datestamp": "2023-08-19 14:53:51", "lastmod": "2023-10-18 20:36:56", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Brink-J", "name": { "family": "Brink", "given": "Jeandrew" } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" }, { "id": "Wasserman-I", "name": { "family": "Wasserman", "given": "Ira" } } ] }, "title": "Nonlinear coupling network to simulate the development of the r-mode instability in neutron stars. I. Construction", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2004 The American Physical Society. \n\nReceived 15 September 2004; published 15 December 2004. \n\nThanks to Harald Pfeiffer for suggestions on the coding of the classes and search algorithms used to manipulate the coupling coefficients and Nikolaos Stergioulas for useful comments. This research is supported in part by NSF Grants No. AST-0307273, No. PHY-9900672, and No. PHY-0312072 at Cornell University.\n\nPublished - PhysRevD.70.124017.pdf
Submitted - 0409048.pdf
", "abstract": "R-modes of a rotating neutron star are unstable because of the emission of gravitational radiation. We explore the saturation amplitudes of these modes determined by nonlinear mode-mode coupling. Modelling the star as incompressible allows the analytic computation of the coupling coefficients. All couplings up to n=30 are obtained, and analytic values for the shear damping and mode normalization are presented. In a subsequent paper we perform numerical simulations of a large set of coupled modes.", "date": "2004-12-15", "date_type": "published", "publication": "Physical Review D", "volume": "70", "number": "12", "publisher": "American Physical Society", "pagerange": "Art. No. 124017", "id_number": "CaltechAUTHORS:20180606-082721678", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180606-082721678", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-0307273" }, { "agency": "NSF", "grant_number": "PHY-9900672" }, { "agency": "NSF", "grant_number": "PHY-0312072" } ] }, "doi": "10.1103/PhysRevD.70.124017", "primary_object": { "basename": "0409048.pdf", "url": "https://authors.library.caltech.edu/records/ddkdw-tk513/files/0409048.pdf" }, "related_objects": [ { "basename": "PhysRevD.70.124017.pdf", "url": "https://authors.library.caltech.edu/records/ddkdw-tk513/files/PhysRevD.70.124017.pdf" } ], "resource_type": "article", "pub_year": "2004", "author_list": "Brink, Jeandrew; Teukolsky, Saul A.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/46sj2-crs97", "eprint_id": 86804, "eprint_status": "archive", "datestamp": "2023-08-19 14:53:45", "lastmod": "2023-10-18 20:36:11", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Brink-J", "name": { "family": "Brink", "given": "Jeandrew" } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" }, { "id": "Wasserman-I", "name": { "family": "Wasserman", "given": "Ira" } } ] }, "title": "Nonlinear couplings of R-modes: Energy transfer and saturation amplitudes at realistic timescales", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2004 The American Physical Society. \n\nReceived 23 June 2004; published 6 December 2004. \n\nThanks are due to Larry Kidder and Harald Pfeiffer for invaluable advice on the numerous technical details required for the development of the codes used. J. B. thanks Alain Cloot and Werner Pesch for many helpful insights about fluids. This research is supported in part by NSF grants AST-0307273, PHY-9900672 and PHY-0312072 at Cornell University.\n\nPublished - PhysRevD.70.121501.pdf
Submitted - 0406085.pdf
", "abstract": "Nonlinear interactions among the inertial modes of a rotating fluid can be described by a network of coupled oscillators. We use such a description for an incompressible fluid to study the development of the r-mode instability of rotating neutron stars. A previous hydrodynamical simulation of the r-mode reported the catastrophic decay of large amplitude r-modes. We explain the dynamics and timescale of this decay analytically by means of a single three mode coupling. We argue that at realistic driving and damping rates such large amplitudes will never actually be reached. By numerically integrating a network of nearly 5000 coupled modes, we find that the linear growth of the r-mode ceases before it reaches an amplitude of around 10^(-4). The lowest parametric instability thresholds for the r-mode are calculated and it is found that the r-mode becomes unstable to modes with 13 < n < 15 if modes up to n = 30 are included. Using the network of coupled oscillators, integration times of 10^6 rotational periods are attainable for realistic values of driving and damping rates. Complicated dynamics of the modal amplitudes are observed. The initial development is governed by the three mode coupling with the lowest parametric instability. Subsequently, a large number of modes are excited, which greatly decreases the linear growth rate of the r-mode.", "date": "2004-12-15", "date_type": "published", "publication": "Physical Review D", "volume": "70", "number": "12", "publisher": "American Physical Society", "pagerange": "Art. No. 121501", "id_number": "CaltechAUTHORS:20180605-144149188", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180605-144149188", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-0307273" }, { "agency": "NSF", "grant_number": "PHY-9900672" }, { "agency": "NSF", "grant_number": "PHY-0312072" } ] }, "doi": "10.1103/PhysRevD.70.121501", "primary_object": { "basename": "PhysRevD.70.121501.pdf", "url": "https://authors.library.caltech.edu/records/46sj2-crs97/files/PhysRevD.70.121501.pdf" }, "related_objects": [ { "basename": "0406085.pdf", "url": "https://authors.library.caltech.edu/records/46sj2-crs97/files/0406085.pdf" } ], "resource_type": "article", "pub_year": "2004", "author_list": "Brink, Jeandrew; Teukolsky, Saul A.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/fd8m8-2ge46", "eprint_id": 1980, "eprint_status": "archive", "datestamp": "2023-08-22 02:03:42", "lastmod": "2023-10-13 23:07:29", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Lindblom-L", "name": { "family": "Lindblom", "given": "Lee" } }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." } }, { "id": "Kidder-L-E", "name": { "family": "Kidder", "given": "Lawrence E." }, "orcid": "0000-0001-5392-7342" }, { "id": "Pfeiffer-H-P", "name": { "family": "Pfeiffer", "given": "Harald P." }, "orcid": "0000-0001-9288-519X" }, { "id": "Shoemaker-D", "name": { "family": "Shoemaker", "given": "Deirdre" } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Controlling the growth of constraints in hyperbolic evolution systems", "ispublished": "pub", "full_text_status": "public", "keywords": "Einstein field equations; Maxwell equations; hyperbolic equations", "note": "\u00a9 2004 The American Physical Society. \n\nReceived 4 February 2004; published 28 June 2004. \n\nWe thank Michael Holst, Oscar Reula, Olivier Sarbach, and Manuel Tiglio for helpful discussions concerning this work. This work was supported in part by NSF grants PHY-0099568 and PHY-0244906 and NASA grants NAG5-10707 and NAG5-12834 at Caltech, and NSF grants PHY-9900672 and PHY-0312072 at Cornell.\n\nPublished - LINprd04.pdf
Submitted - 0402027.pdf
", "abstract": "Motivated by the need to control the exponential growth of constraint violations in numerical solutions of the Einstein evolution equations, two methods are studied here for controlling this growth in general hyperbolic evolution systems. The first method adjusts the evolution equations dynamically, by adding multiples of the constraints, in a way designed to minimize this growth. The second method imposes special constraint preserving boundary conditions on the incoming components of the dynamical fields. The efficacy of these methods is tested by using them to control the growth of constraints in fully dynamical 3D numerical solutions of a particular representation of the Maxwell equations that is subject to constraint violations. The constraint preserving boundary conditions are found to be much more effective than active constraint control in the case of this Maxwell system.", "date": "2004-06-15", "date_type": "published", "publication": "Physical Review D", "volume": "69", "number": "12", "publisher": "American Physical Society", "pagerange": "Art. No. 124025", "id_number": "CaltechAUTHORS:LINprd04", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:LINprd04", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY-0099568" }, { "agency": "NSF", "grant_number": "PHY-0244906" }, { "agency": "NASA", "grant_number": "NAG5-10707" }, { "agency": "NASA", "grant_number": "NAG5-12834" }, { "agency": "NSF", "grant_number": "PHY-9900672" }, { "agency": "NSF", "grant_number": "PHY-0312072" } ] }, "local_group": { "items": [ { "id": "TAPIR" } ] }, "doi": "10.1103/PhysRevD.69.124025", "primary_object": { "basename": "LINprd04.pdf", "url": "https://authors.library.caltech.edu/records/fd8m8-2ge46/files/LINprd04.pdf" }, "related_objects": [ { "basename": "0402027.pdf", "url": "https://authors.library.caltech.edu/records/fd8m8-2ge46/files/0402027.pdf" } ], "resource_type": "article", "pub_year": "2004", "author_list": "Lindblom, Lee; Scheel, Mark A.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/k4r9h-3c561", "eprint_id": 1947, "eprint_status": "archive", "datestamp": "2023-08-22 01:57:00", "lastmod": "2023-10-13 23:06:21", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." } }, { "id": "Erickcek-A-L", "name": { "family": "Erickcek", "given": "Adrienne L." } }, { "id": "Burko-L-M", "name": { "family": "Burko", "given": "Lior M." } }, { "id": "Kidder-L-E", "name": { "family": "Kidder", "given": "Lawrence E." }, "orcid": "0000-0001-5392-7342" }, { "id": "Pfeiffer-H-P", "name": { "family": "Pfeiffer", "given": "Harald P." }, "orcid": "0000-0001-9288-519X" }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "3D simulations of linearized scalar fields in Kerr spacetime", "ispublished": "pub", "full_text_status": "public", "keywords": "space-time configurations; black holes; perturbation theory", "note": "\u00a9 2004 The American Physical Society. \n\n(Received 6 May 2003; published 12 May 2004) \n\nWe thank Lee Lindblom and Richard Price for valuable discussions. Some computations were performed on the IA-32 Linux cluster at NCSA. This research was supported in part by NSF grant PHY-0099568 at the California Institute of Technology, NSF grant PHY-9900672 at Cornell University, and NSF grants PHY-9734871 and PHY-0244605 at the University of Utah. A.L.E. was supported by the LIGO Summer Undergraduate Research Program at the California Institute of Technology. L.M.B. thanks Kip Thorne for hospitality at Caltech during the beginning phase of this work.\n\nPublished - SCHEprd04.pdf
Submitted - 0305027.pdf
", "abstract": "We investigate the behavior of a dynamical scalar field on a fixed Kerr background in Kerr-Schild coordinates using a (3+1)-dimensional spectral evolution code, and we measure the power-law tail decay that occurs at late times. We compare evolutions of initial data proportional to f(r)Y[script l]m(theta,phi), where Y[script l]m is a spherical harmonic and (r,theta,phi) are Kerr-Schild coordinates, to that of initial data proportional to f(rBL)Y[script l]m(thetaBL,phi), where (rBL,thetaBL) are Boyer-Lindquist coordinates. We find that although these two cases are initially almost identical, the evolution can be quite different at intermediate times; however, at late times the power-law decay rates are equal.", "date": "2004-05-15", "date_type": "published", "publication": "Physical Review D", "volume": "69", "number": "10", "publisher": "American Physical Society", "pagerange": "Art. No. 104006", "id_number": "CaltechAUTHORS:SCHEprd04", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:SCHEprd04", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY-0099568" }, { "agency": "NSF", "grant_number": "PHY-9900672" }, { "agency": "NSF", "grant_number": "PHY-9734871" }, { "agency": "NSF", "grant_number": "PHY-0244605" }, { "agency": "Caltech Summer Undergraduate Research Fellowship (SURF)" } ] }, "local_group": { "items": [ { "id": "TAPIR" } ] }, "doi": "10.1103/PhysRevD.69.104006", "primary_object": { "basename": "0305027.pdf", "url": "https://authors.library.caltech.edu/records/k4r9h-3c561/files/0305027.pdf" }, "related_objects": [ { "basename": "SCHEprd04.pdf", "url": "https://authors.library.caltech.edu/records/k4r9h-3c561/files/SCHEprd04.pdf" } ], "resource_type": "article", "pub_year": "2004", "author_list": "Scheel, Mark A.; Erickcek, Adrienne L.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/vjqmq-pkz81", "eprint_id": 86811, "eprint_status": "archive", "datestamp": "2023-08-22 00:43:24", "lastmod": "2023-10-18 20:36:27", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Arras-P", "name": { "family": "Arras", "given": "Phil" } }, { "id": "Flanagan-\u00c9-\u00c9", "name": { "family": "Flanagan", "given": "Eanna E." } }, { "id": "Morsink-S-M", "name": { "family": "Morsink", "given": "Sharon M." }, "orcid": "0000-0003-4357-0575" }, { "id": "Schenk-A-K", "name": { "family": "Schenk", "given": "A. Katrin" } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" }, { "id": "Wasserman-I", "name": { "family": "Wasserman", "given": "Ira" } } ] }, "title": "Saturation of the r-Mode Instability", "ispublished": "pub", "full_text_status": "public", "keywords": "gravitational waves; stars: neutron; stars: oscillations; turbulence", "note": "\u00a9 2003. The American Astronomical Society. \n\nReceived 2002 February 18; accepted 2003 February 4. \n\nIt is a pleasure to acknowledge many useful conversations on stellar oscillations with Yanqin Wu. P. A. would also like to thank Chris Matzner, Chris Thompson, and Maxim Lyutikov. Part of this work was completed when two of us (P. A. and S. M.) were at the Institute for Theoretical Physics at the Spin and Magnetism in Young Neutron Stars workshop. We thank Lars Bildsten for his gracious hospitality and for a number of useful conversations and John Friedman, Curt Cutler, and Peter Goldreich for useful comments on the manuscript. P. A. is supported by an NSERC Fellowship. This work was supported in part by NSF grants PHY 99-00672 and PHY 00-84729 at Cornell University. E. E. F. was supported by NSF grants PHY 97-22189 and PHY 01-40209 and by the Alfred P. Sloan Foundation. S. M. received support from NSERC.\n\nPublished - Arras_2003_ApJ_591_1129.pdf
Accepted Version - 0202345.pdf
", "abstract": "Rossby waves (r-modes) in rapidly rotating neutron stars are unstable because of the emission of gravitational radiation. As a result, the stellar rotational energy is converted into both gravitational waves and r-mode energy. The saturation level for the r-mode energy is a fundamental parameter needed to determine how fast the neutron star spins down, as well as whether gravitational waves will be detectable. In this paper we study saturation by nonlinear transfer of energy to the sea of stellar \"inertial\" oscillation modes that arise in rotating stars with negligible buoyancy and elastic restoring forces. We present detailed calculations of stellar inertial modes in the WKB limit, their linear damping by bulk and shear viscosity, and the nonlinear coupling forces among these modes. The saturation amplitude is derived in the extreme limits of strong or weak driving by radiation reaction, as compared to the damping rate of low-order inertial modes. In the weak driving case, energy can be stably transferred to a small number of modes, which damp the energy as heat or neutrinos. In the strong driving case, we show that a turbulent cascade develops, with a constant flux of energy to large wavenumbers and small frequencies where it is damped by shear viscosity. We find that the saturation energy is extremely small, at least 4 orders of magnitude smaller than that found by previous investigators. We show that the large saturation energy found in the simulations of Lindblom and coworkers is an artifact of their unphysically large radiation reaction force. In most physical situations of interest, for either nascent, rapidly rotating neutron stars or neutron stars being spun up by accretion in low-mass X-ray binaries (LMXBs), the strong driving limit is appropriate and the saturation energy is roughly E_(r-mode)/(0.5Mr^2_+\u03a9^2) sime 0.1\u03b3gr/\u03a9 \u2243 10^(-6)(\u03bd_(spin)/10^3 Hz)^5, where M and r* are the stellar mass and radius, respectively, \u03b3_(gr) is the driving rate by gravitational radiation, \u03a9 is the angular velocity of the star, and \u03bd_(spin) is the spin frequency. At such a low saturation amplitude, the characteristic time for the star to exit the region of r-mode instability is \u2273 10^3-10^4 yr, depending sensitively on the instability curve. Although our saturation amplitude is smaller than that found by previous investigators, it is still sufficiently large to explain the observed period clustering in LMXBs. We find that the r-mode signal from both newly born neutron stars and LMXBs in the spin-down phase of Levin's limit cycle will be detectable by enhanced LIGO detectors out to ~100-200 kpc.", "date": "2003-07-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "591", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1129-1151", "id_number": "CaltechAUTHORS:20180605-155948780", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180605-155948780", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "NSF", "grant_number": "PHY 99-00672" }, { "agency": "NSF", "grant_number": "PHY 00-84729" }, { "agency": "NSF", "grant_number": "PHY 97-22189" }, { "agency": "NSF", "grant_number": "PHY 01-40209" }, { "agency": "Alfred P. Sloan Foundation" } ] }, "doi": "10.1086/374657", "primary_object": { "basename": "Arras_2003_ApJ_591_1129.pdf", "url": "https://authors.library.caltech.edu/records/vjqmq-pkz81/files/Arras_2003_ApJ_591_1129.pdf" }, "related_objects": [ { "basename": "0202345.pdf", "url": "https://authors.library.caltech.edu/records/vjqmq-pkz81/files/0202345.pdf" } ], "resource_type": "article", "pub_year": "2003", "author_list": "Arras, Phil; Flanagan, Eanna E.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/xkeav-9k261", "eprint_id": 86812, "eprint_status": "archive", "datestamp": "2023-08-22 00:30:54", "lastmod": "2023-10-18 20:36:30", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Pfeiffer-H-P", "name": { "family": "Pfeiffer", "given": "Harald P." }, "orcid": "0000-0001-9288-519X" }, { "id": "Kidder-L-E", "name": { "family": "Kidder", "given": "Lawrence E." }, "orcid": "0000-0001-5392-7342" }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "A multidomain spectral method for solving elliptic equations", "ispublished": "pub", "full_text_status": "public", "keywords": "Spectral methods; Domain decomposition; Elliptic partial differential equations; General relativity; Initial value problem", "note": "\u00a9 2002 Elsevier. \n\nReceived 19 July 2002, Accepted 15 October 2002, Available online 30 January 2003. \n\nWe thank Gregory Cook for helpful discussions. This work was supported in part by NSF grants PHY-9800737 and PHY-9900672 to Cornell University. Computations were performed on the IBM SP2 of the Department of Physics, Wake Forest University, with support from an IBM SUR grant, as well as on the Platinum cluster of NCSA.\n\nSubmitted - 0202096.pdf
", "abstract": "We present a new solver for coupled nonlinear elliptic partial differential equations (PDEs). The solver is based on pseudo-spectral collocation with domain decomposition and can handle one- to three-dimensional problems. It has three distinct features. First, the combined problem of solving the PDE, satisfying the boundary conditions, and matching between different subdomains is cast into one set of equations readily accessible to standard linear and nonlinear solvers. Second, touching as well as overlapping subdomains are supported; both rectangular blocks with Chebyshev basis functions as well as spherical shells with an expansion in spherical harmonics are implemented. Third, the code is very flexible: The domain decomposition as well as the distribution of collocation points in each domain can be chosen at run time, and the solver is easily adaptable to new PDEs. The code has been used to solve the equations of the initial value problem of general relativity and should be useful in many other problems. We compare the new method to finite difference codes and find it superior in both runtime and accuracy, at least for the smooth problems considered here.", "date": "2003-05-15", "date_type": "published", "publication": "Computer Physics Communications", "volume": "152", "number": "3", "publisher": "Elsevier", "pagerange": "253-273", "id_number": "CaltechAUTHORS:20180605-160909307", "issn": "0010-4655", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180605-160909307", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY-9800737" }, { "agency": "NSF", "grant_number": "PHY-9900672" }, { "agency": "IBM" } ] }, "doi": "10.1016/S0010-4655(02)00847-0", "primary_object": { "basename": "0202096.pdf", "url": "https://authors.library.caltech.edu/records/xkeav-9k261/files/0202096.pdf" }, "resource_type": "article", "pub_year": "2003", "author_list": "Pfeiffer, Harald P.; Kidder, Lawrence E.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/t3tyv-81923", "eprint_id": 86810, "eprint_status": "archive", "datestamp": "2023-08-19 11:04:39", "lastmod": "2024-01-14 20:14:25", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Numerical relativity: maximizing the scientific payoff from gravitational wave detection", "ispublished": "unpub", "full_text_status": "public", "keywords": "Einstein's equations, gravitational waves, black holes, neutron stars", "note": "\u00a9 2003 Society of Photo-Optical Instrumentation Engineers (SPIE). \n\nThe work described here was carried out with my collaborators, Phil Arras, Eanna Flanagan, Larry Kidder, Sharon Morsink, Mark Scheel, Katrin Schenk, and Ira Wasserman. This work was supported in part by NSF grants PHY-9900672 and PHY-0084729 at Cornell University.\n\nPublished - 116.pdf
", "abstract": "For many of the proposed LIGO sources, we are currently unable to produce reliable theoretical waveforms or event rates. Usually the difficulty is in performing numerical simulations. These problems seriously undermine our ability to extract science from LIGO, or in some cases even to detect sources at all. We describe two sources where these problems are present: the merger of a binary black hole system, and a newborn neutron star unstable to r-modes. We explain the origin of the difficulties, and how they might be overcome.", "date": "2003-02-26", "date_type": "published", "publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)", "place_of_pub": "Bellingham, WA", "pagerange": "116-122", "id_number": "CaltechAUTHORS:20180605-155224023", "isbn": "0819446351", "book_title": "Gravitational-Wave Detection", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180605-155224023", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY-9900672" }, { "agency": "NSF", "grant_number": "PHY-0084729" } ] }, "contributors": { "items": [ { "id": "Saulson-P-R", "name": { "family": "Saulson", "given": "Peter" } }, { "id": "Cruise-M", "name": { "family": "Cruise", "given": "Mike" } } ] }, "doi": "10.1117/12.459025", "primary_object": { "basename": "116.pdf", "url": "https://authors.library.caltech.edu/records/t3tyv-81923/files/116.pdf" }, "resource_type": "book_section", "pub_year": "2003", "author_list": "Teukolsky, Saul A." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/6gcz5-q4109", "eprint_id": 3017, "eprint_status": "archive", "datestamp": "2023-08-21 23:57:32", "lastmod": "2023-10-16 15:33:58", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." } }, { "id": "Kidder-L-E", "name": { "family": "Kidder", "given": "Lawrence E." }, "orcid": "0000-0001-5392-7342" }, { "id": "Lindblom-L", "name": { "family": "Lindblom", "given": "Lee" } }, { "id": "Pfeiffer-H-P", "name": { "family": "Pfeiffer", "given": "Harald P." }, "orcid": "0000-0001-9288-519X" }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Toward stable 3D numerical evolutions of black-hole spacetimes", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2002 The American Physical Society. \n\nReceived 30 September 2002; published 17 December 2002. \n\nSome computations were performed on the IA-32 Linux cluster at NCSA. This research was supported in part by NSF grant PHY-0099568 and NASA grant NAG5-10707 at California Institute of Technology and NSF grants PHY-9800737 and PHY-9900672 at Cornell University.\n\nPublished - SCHEprd02.pdf
Submitted - 0209115.pdf
", "abstract": "Three dimensional (3D) numerical evolutions of static black holes with excision are presented. These evolutions extend to about 8000M, where M is the mass of the black hole. This degree of stability is achieved by using growth-rate estimates to guide the fine tuning of the parameters in a multiparameter family of symmetric hyperbolic representations of the Einstein evolution equations. These evolutions were performed using a fixed gauge in order to separate the intrinsic stability of the evolution equations from the effects of stability-enhancing gauge choices.", "date": "2002-12-15", "date_type": "published", "publication": "Physical Review D", "volume": "66", "number": "12", "publisher": "American Physical Society", "pagerange": "Art. No. 124005", "id_number": "CaltechAUTHORS:SCHEprd02", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:SCHEprd02", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY-0099568" }, { "agency": "NASA", "grant_number": "NAG5-10707" }, { "agency": "NSF", "grant_number": "PHY-9800737" }, { "agency": "NSF", "grant_number": "PHY-9900672" } ] }, "local_group": { "items": [ { "id": "TAPIR" } ] }, "doi": "10.1103/PhysRevD.66.124005", "primary_object": { "basename": "0209115.pdf", "url": "https://authors.library.caltech.edu/records/6gcz5-q4109/files/0209115.pdf" }, "related_objects": [ { "basename": "SCHEprd02.pdf", "url": "https://authors.library.caltech.edu/records/6gcz5-q4109/files/SCHEprd02.pdf" } ], "resource_type": "article", "pub_year": "2002", "author_list": "Scheel, Mark A.; Kidder, Lawrence E.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/z6hmg-ktz25", "eprint_id": 86805, "eprint_status": "archive", "datestamp": "2023-08-19 09:49:26", "lastmod": "2023-10-18 20:36:14", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Pfeiffer-H-P", "name": { "family": "Pfeiffer", "given": "Harald P." }, "orcid": "0000-0001-9288-519X" }, { "id": "Cook-G-B", "name": { "family": "Cook", "given": "Gregory B." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Comparing initial-data sets for binary black holes", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2002 The American Physical Society. \n\nReceived 25 March 2002; published 31 July 2002. \n\nWe thank Lawrence Kidder, Mark Scheel, and James York for helpful discussions. This work was supported in part by NSF grants PHY-9800737 and PHY-9900672 to Cornell University, and by NSF grant PHY-9988581 to Wake Forest University. Computations were performed on the IBM SP2 of the Department of Physics, Wake Forest University, with support from an IBM SUR grant.\n\nPublished - PhysRevD.66.024047.pdf
Accepted Version - 0203085.pdf
", "abstract": "We compare the results of constructing binary black hole initial data with three different decompositions of the constraint equations of general relativity. For each decomposition we compute the initial data using a superposition of two Kerr-Schild black holes to fix the freely specifiable data. We find that these initial-data sets differ significantly, with the ADM energy varying by as much as 5% of the total mass. We find that all initial-data sets currently used for evolutions might contain unphysical gravitational radiation of the order of several percent of the total mass. This is comparable to the amount of gravitational-wave energy observed during the evolved collision. More astrophysically realistic initial data will require more careful choices of the freely specifiable data and boundary conditions for both the metric and extrinsic curvature. However, we find that the choice of extrinsic curvature affects the resulting data sets more strongly than the choice of conformal metric.", "date": "2002-07-15", "date_type": "published", "publication": "Physical Review D", "volume": "66", "number": "2", "publisher": "American Physical Society", "pagerange": "Art. No. 024047", "id_number": "CaltechAUTHORS:20180605-144741747", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180605-144741747", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY-9800737" }, { "agency": "NSF", "grant_number": "PHY-9900672" }, { "agency": "NSF", "grant_number": "PHY-9988581" }, { "agency": "IBM" } ] }, "doi": "10.1103/PhysRevD.66.024047", "primary_object": { "basename": "0203085.pdf", "url": "https://authors.library.caltech.edu/records/z6hmg-ktz25/files/0203085.pdf" }, "related_objects": [ { "basename": "PhysRevD.66.024047.pdf", "url": "https://authors.library.caltech.edu/records/z6hmg-ktz25/files/PhysRevD.66.024047.pdf" } ], "resource_type": "article", "pub_year": "2002", "author_list": "Pfeiffer, Harald P.; Cook, Gregory B.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/vs8tv-d0d26", "eprint_id": 86802, "eprint_status": "archive", "datestamp": "2023-08-19 08:57:59", "lastmod": "2023-10-18 20:36:03", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Schenk-A-K", "name": { "family": "Schenk", "given": "A. K." } }, { "id": "Arras-P", "name": { "family": "Arras", "given": "P." } }, { "id": "Flanagan-\u00c9-\u00c9", "name": { "family": "Flanagan", "given": "\u00c9. \u00c9." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "S. A." }, "orcid": "0000-0001-9765-4526" }, { "id": "Wasserman-I", "name": { "family": "Wasserman", "given": "I." } } ] }, "title": "Nonlinear mode coupling in rotating stars and the r-mode instability in neutron stars", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2001 The American Physical Society. \n\nReceived 25 January 2001; revised manuscript received 10 July 2001; published 29 November 2001. \n\nThis work was supported in part by NSF grants PHY-9900672 and PHY-9722189 and NASA grants NAG5-7264 and NAG5-8356 to Cornell University. E.F. received support from the Alfred P. Sloan Foundation. P. A. wishes to thank Yanqin Wu and Chris Matzner for many useful conversations. We thank Larry Kidder, Dong Lai, Sharon Morsink, and Mark Scheel for useful conversations, and Sharon Morsink for detailed and helpful suggestions on the manuscript.\n\nPublished - PhysRevD.65.024001.pdf
Submitted - 0101092.pdf
", "abstract": "We develop the formalism required to study the nonlinear interaction of modes in rotating Newtonian stars, assuming that the mode amplitudes are only mildly nonlinear. The formalism is simpler than previous treatments of mode-mode interactions for spherical stars, and simplifies and corrects previous treatments for rotating stars. At linear order, we elucidate and extend slightly a formalism due to Schutz, show how to decompose a general motion of a rotating star into a sum over modes, and obtain uncoupled equations of motion for the mode amplitudes under the influence of an external force. Nonlinear effects are added perturbatively via three-mode couplings, which suffices for moderate amplitude modal excitations; the formalism is easy to extend to higher order couplings. We describe a new, efficient way to compute the modal coupling coefficients, to zeroth order in the stellar rotation rate, using spin-weighted spherical harmonics. The formalism is general enough to allow computation of the initial trends in the evolution of the spin frequency and differential rotation of the background star. We apply this formalism to derive some properties of the coupling coefficients relevant to the nonlinear interactions of unstable r modes in neutron stars, postponing numerical integrations of the coupled equations of motion to a later paper. First, we clarify some aspects of the expansion in stellar rotation frequency \u03a9 that is often used to compute approximate mode functions. We show that, in zero-buoyancy stars, the rotational modes (those modes whose frequencies vanish as \u03a9 \u2192 0) are orthogonal to zeroth order in \u03a9. From an astrophysical viewpoint, the most interesting result of this paper is that many couplings of r modes to other rotational modes are small: either they vanish altogether because of various selection rules, or they vanish to lowest order in \u03a9 or in compressibility. In particular, in zero-buoyancy stars, the coupling of three r modes is forbidden entirely and the coupling of two r modes to one hybrid, or r-g rotational, mode vanishes to zeroth order in rotation frequency. The coupling of any three rotational modes vanishes to zeroth order in compressibility and in \u03a9. In nonzero-buoyancy stars, coupling of the r modes to each other vanishes to zeroth order in \u03a9. Couplings to regular modes (those modes whose frequencies are finite in the limit \u03a9 \u2192 0),such as f modes, are not zero, but since the natural frequencies of these modes are relatively large in the slow rotation limit compared to those of the r modes, energy transfer to those modes is not expected to be efficient.", "date": "2002-01-15", "date_type": "published", "publication": "Physical Review D", "volume": "65", "number": "2", "publisher": "American Physical Society", "pagerange": "Art. No. 024001", "id_number": "CaltechAUTHORS:20180605-142812514", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180605-142812514", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY-9900672" }, { "agency": "NSF", "grant_number": "PHY-9722189" }, { "agency": "NASA", "grant_number": "NAG5-7264" }, { "agency": "NASA", "grant_number": "NAG5-8356" }, { "agency": "Alfred P. Sloan Foundation" } ] }, "collection": "CaltechAUTHORS", "doi": "10.1103/PhysRevD.65.024001", "primary_object": { "basename": "PhysRevD.65.024001.pdf", "url": "https://authors.library.caltech.edu/records/vs8tv-d0d26/files/PhysRevD.65.024001.pdf" }, "related_objects": [ { "basename": "0101092.pdf", "url": "https://authors.library.caltech.edu/records/vs8tv-d0d26/files/0101092.pdf" } ], "resource_type": "article", "pub_year": "2002", "author_list": "Schenk, A. K.; Arras, P.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/bpd6q-f5756", "eprint_id": 86809, "eprint_status": "archive", "datestamp": "2023-08-19 08:17:47", "lastmod": "2023-10-18 20:36:22", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kidder-L-E", "name": { "family": "Kidder", "given": "Lawrence E." }, "orcid": "0000-0001-5392-7342" }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Extending the lifetime of 3D black hole computations with a new hyperbolic system of evolution equations", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2001 American Physical Society. \n\n(Received 8 May 2001; published 27 August 2001) \n\nWe thank Harald Pfeiffer, Manuel Tiglio, and James W. York, Jr. for helpful discussions. This work was supported in part by NSF Grant Nos. PHY-9900672 and PHY-0084729 and NASA Grant No. NAG5-7264. Computations were performed on the National Computational Science Alliance SGI Origin 2000, and on the Wake Forest University Department of Physics IBM SP2 with support from an IBM SUR grant.\n\nPublished - PhysRevD.64.064017.pdf
Submitted - 0105031.pdf
", "abstract": "We present a new many-parameter family of hyperbolic representations of Einstein's equations, which we obtain by a straightforward generalization of previously known systems. We solve the resulting evolution equations numerically for a Schwarzschild black hole in three spatial dimensions, and find that the stability of the simulation is strongly dependent on the form of the equations (i.e. the choice of parameters of the hyperbolic system), independent of the numerics. For an appropriate range of parameters we can evolve a single three-dimensional black hole to t \u2243 600 M \u2013 1300 M, and we are apparently limited by constraint-violating solutions of the evolution equations. We expect that our method should result in comparable times for evolutions of a binary black hole system.", "date": "2001-09-15", "date_type": "published", "publication": "Physical Review D", "volume": "64", "number": "6", "publisher": "American Physical Society", "pagerange": "Art. No. 064017", "id_number": "CaltechAUTHORS:20180605-154731644", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180605-154731644", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY-9900672" }, { "agency": "NSF", "grant_number": "PHY-0084729" }, { "agency": "NASA", "grant_number": "NAG5-7264" }, { "agency": "IBM" } ] }, "doi": "10.1103/PhysRevD.64.064017", "primary_object": { "basename": "0105031.pdf", "url": "https://authors.library.caltech.edu/records/bpd6q-f5756/files/0105031.pdf" }, "related_objects": [ { "basename": "PhysRevD.64.064017.pdf", "url": "https://authors.library.caltech.edu/records/bpd6q-f5756/files/PhysRevD.64.064017.pdf" } ], "resource_type": "article", "pub_year": "2001", "author_list": "Kidder, Lawrence E.; Scheel, Mark A.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/5ytnh-02m65", "eprint_id": 86808, "eprint_status": "archive", "datestamp": "2023-09-15 05:54:29", "lastmod": "2023-10-23 21:22:03", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Pfeiffer-H-P", "name": { "family": "Pfeiffer", "given": "Harald P." }, "orcid": "0000-0001-9288-519X" }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" }, { "id": "Cook-G-B", "name": { "family": "Cook", "given": "Gregory B." } } ] }, "title": "Quasicircular orbits for spinning binary black holes", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2000 American Physical Society. \n\n(Received 22 June 2000; published 19 October 2000) \n\nWe thank Larry Kidder and Mark Scheel for helpful discussions. This work was supported in part by NSF grants PHY-9800737 and PHY-9900672 and NASA grant NAG5-7264 to Cornell University and NSF grant PHY-9988581 to Wake Forest University. Computations were performed on the IBM SP2 at Cornell Theory Center and on the Wake Forest University Department of Physics IBM SP2 with support from an IBM SUR grant.\n\nPublished - PhysRevD.62.104018.pdf
Submitted - 0006084
", "abstract": "Using an effective potential method we examine binary black holes where the individual holes carry spin. We trace out sequences of quasi-circular orbits and locate the innermost stable circular orbit (ISCO) as a function of spin. At large separations, the sequences of quasi-circular orbits match well with post-Newtonian expansions, although a clear signature of the simplifying assumption of conformal flatness is seen. The position of the ISCO is found to be strongly dependent on the magnitude of the spin on each black hole. At close separations of the holes, the effective potential method breaks down. In all cases where an ISCO could be determined, we found that an apparent horizon encompassing both holes forms for separations well inside the ISCO. Nevertheless, we argue that the formation of a common horizon is still associated with the breakdown of the effective potential method.", "date": "2000-11-15", "date_type": "published", "publication": "Physical Review D", "volume": "62", "number": "10", "publisher": "American Physical Society", "pagerange": "Art. No. 104018", "id_number": "CaltechAUTHORS:20180605-154306927", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180605-154306927", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY-9800737" }, { "agency": "NSF", "grant_number": "PHY-9900672" }, { "agency": "NASA", "grant_number": "NAG5-7264" }, { "agency": "NSF", "grant_number": "PHY-9988581" }, { "agency": "IBM" } ] }, "doi": "10.1103/PhysRevD.62.104018", "primary_object": { "basename": "PhysRevD.62.104018.pdf", "url": "https://authors.library.caltech.edu/records/5ytnh-02m65/files/PhysRevD.62.104018.pdf" }, "related_objects": [ { "basename": "0006084", "url": "https://authors.library.caltech.edu/records/5ytnh-02m65/files/0006084" } ], "resource_type": "article", "pub_year": "2000", "author_list": "Pfeiffer, Harald P.; Teukolsky, Saul A.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/s7s8k-c1a65", "eprint_id": 86807, "eprint_status": "archive", "datestamp": "2023-08-19 06:26:11", "lastmod": "2023-10-18 20:36:19", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kidder-L-E", "name": { "family": "Kidder", "given": "Lawrence E." }, "orcid": "0000-0001-5392-7342" }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" }, { "id": "Carlson-E-D", "name": { "family": "Carlson", "given": "Eric D." } }, { "id": "Cook-G-B", "name": { "family": "Cook", "given": "Gregory B." } } ] }, "title": "Black hole evolution by spectral methods", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2000 American Physical Society. \n\n(Received 15 May 2000; published 26 September 2000) \n\nThis work was supported in part by NSF grants PHY-9800737 and PHY-9900672 and NASA grant NAG5-7264 to Cornell University, and NSF grants PHY-9802571 and PHY-9988581 to Wake Forest University. Computations were performed on the National Computational Science Alliance SGI Origin2000, and on the Wake Forest University Department of Physics IBM SP2 with support from an IBM SUR grant.\n\nPublished - PhysRevD.62.084032.pdf
Submitted - 0005056.pdf
", "abstract": "Current methods of evolving a spacetime containing one or more black holes are plagued by instabilities that prohibit long-term evolution. Some of these instabilities may be due to the numerical method used, traditionally finite differencing. In this paper, we explore the use of a pseudospectral collocation (PSC) method for the evolution of a spherically symmetric black hole spacetime in one dimension using a hyperbolic formulation of Einstein's equations. We demonstrate that our PSC method is able to evolve a spherically symmetric black hole spacetime forever without enforcing constraints, even if we add dynamics via a Klein-Gordon scalar field. We find that, in contrast with finite-differencing methods, black hole excision is a trivial operation using PSC applied to a hyperbolic formulation of Einstein's equations. We discuss the extension of this method to three spatial dimensions.", "date": "2000-10-15", "date_type": "published", "publication": "Physical Review D", "volume": "62", "number": "8", "publisher": "American Physical Society", "pagerange": "Art. no. 084032", "id_number": "CaltechAUTHORS:20180605-153821098", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180605-153821098", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY-9800737" }, { "agency": "NSF", "grant_number": "PHY-9900672" }, { "agency": "NASA", "grant_number": "NAG5-7264" }, { "agency": "NSF", "grant_number": "PHY-9802571" }, { "agency": "NSF", "grant_number": "PHY-9988581" }, { "agency": "IBM" } ] }, "doi": "10.1103/PhysRevD.62.084032", "primary_object": { "basename": "0005056.pdf", "url": "https://authors.library.caltech.edu/records/s7s8k-c1a65/files/0005056.pdf" }, "related_objects": [ { "basename": "PhysRevD.62.084032.pdf", "url": "https://authors.library.caltech.edu/records/s7s8k-c1a65/files/PhysRevD.62.084032.pdf" } ], "resource_type": "article", "pub_year": "2000", "author_list": "Kidder, Lawrence E.; Scheel, Mark A.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/kxw9r-ymm76", "eprint_id": 86806, "eprint_status": "archive", "datestamp": "2023-08-19 05:39:25", "lastmod": "2023-10-18 20:36:17", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Stability of the iterated Crank-Nicholson method in numerical relativity", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2000 American Physical Society. \n\n(Received 7 September 1999; published 14 March 2000) \n\nThis work was supported in part by NSF grant PHY 99-00672 and NASA Grant NAG5-7264 to Cornell University.\n\nPublished - PhysRevD.61.087501.pdf
Submitted - 9909026.pdf
", "abstract": "The iterated Crank-Nicholson method has become a popular algorithm in numerical relativity. We show that one should carry out exactly two iterations and no more. While the limit of an infinite number of iterations is the standard Crank-Nicholson method, it can in fact be worse to do more than two iterations, and it never helps. We explain how this paradoxical result arises.", "date": "2000-04-15", "date_type": "published", "publication": "Physical Review D", "volume": "61", "number": "8", "publisher": "American Physical Society", "pagerange": "Art. No. 087501", "id_number": "CaltechAUTHORS:20180605-153229640", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180605-153229640", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY 99-00672" }, { "agency": "NASA", "grant_number": "NAG5-7264" } ] }, "doi": "10.1103/PhysRevD.61.087501", "primary_object": { "basename": "9909026.pdf", "url": "https://authors.library.caltech.edu/records/kxw9r-ymm76/files/9909026.pdf" }, "related_objects": [ { "basename": "PhysRevD.61.087501.pdf", "url": "https://authors.library.caltech.edu/records/kxw9r-ymm76/files/PhysRevD.61.087501.pdf" } ], "resource_type": "article", "pub_year": "2000", "author_list": "Teukolsky, Saul A." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/bs2r8-jzg12", "eprint_id": 87490, "eprint_status": "archive", "datestamp": "2023-08-22 13:57:31", "lastmod": "2023-10-18 21:13:03", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Schenk-A-K", "name": { "family": "Schenk", "given": "A. Katrin" } }, { "id": "Shapiro-S-L", "name": { "family": "Shapiro", "given": "Stuart L." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Hot, Rotating Disks in General Relativity: Collisionless Equilibrium Models", "ispublished": "pub", "full_text_status": "public", "keywords": "accretion, accretion disks; relativity", "note": "\u00a9 1999. The American Astronomical Society. \n\nReceived 1998 January 15; accepted 1999 March 16. \n\n We thank Mark Scheel and Greg Cook for useful discussions. We also thank Greg Cook for generously sharing a computer code with us. This work has been supported in part by National Science Foundation grant PHY 94-08378 at Cornell University, and by National Science Foundation grant AST 96-18524 and NASA grant NAG 5-3420 at the University of Illinois at Urbana-Champaign.\n\nPublished - Schenk_1999_ApJ_521_310.pdf
Submitted - 9801056.pdf
", "abstract": "We present a method for constructing equilibrium disks with net angular momentum in general relativity. The method solves the relativistic Vlasov equation coupled to Einstein's equations for the gravitational field. We apply the method to construct disks that are relativistic versions of Newtonian Kalnajs disks. In Newtonian gravity these disks are analytic and are stable against ring formation for certain ranges of their velocity dispersion. We investigate the existence of fully general relativistic equilibrium sequences for differing values of the velocity dispersion. These models are the first rotating, relativistic disk solutions of the collisionless Boltzmann equation.", "date": "1999-08-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "521", "number": "1", "publisher": "American Astronomical Society", "pagerange": "310-318", "id_number": "CaltechAUTHORS:20180629-150830138", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180629-150830138", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY 94-08378" }, { "agency": "NSF", "grant_number": "AST 96-18524" }, { "agency": "NASA", "grant_number": "NAG 5-3420" } ] }, "doi": "10.1086/307510", "primary_object": { "basename": "Schenk_1999_ApJ_521_310.pdf", "url": "https://authors.library.caltech.edu/records/bs2r8-jzg12/files/Schenk_1999_ApJ_521_310.pdf" }, "related_objects": [ { "basename": "9801056.pdf", "url": "https://authors.library.caltech.edu/records/bs2r8-jzg12/files/9801056.pdf" } ], "resource_type": "article", "pub_year": "1999", "author_list": "Schenk, A. Katrin; Shapiro, Stuart L.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/ee14h-j0v36", "eprint_id": 87492, "eprint_status": "archive", "datestamp": "2023-08-19 04:19:34", "lastmod": "2023-10-18 21:13:08", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Horowitz-G-T", "name": { "family": "Horowitz", "given": "Gary T." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Black holes", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 1999 American Physical Society. \n\nWe thank Ramesh Narayan for helpful discussions. This work was supported in part by NSF Grants PHY95-07065 at Santa Barbara and PHY 94-08378 at Cornell University.\n\nPublished - RevModPhys.71.S180.pdf
Submitted - 9808035.pdf
", "abstract": "Black holes are among the most intriguing objects in modern physics. They power quasars and other active galactic nuclei and also provide key insights into quantum gravity. We review the observational evidence for black holes and briefly discuss some of their properties. We also describe some recent developments involving cosmic censorship and the statistical origin of black-hole entropy.", "date": "1999-05", "date_type": "published", "publication": "Reviews of Modern Physics", "volume": "71", "number": "2", "publisher": "American Physical Society", "pagerange": "S180-S186", "id_number": "CaltechAUTHORS:20180629-152251147", "issn": "0034-6861", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180629-152251147", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY 95-07065" }, { "agency": "NSF", "grant_number": "PHY 94-08378" } ] }, "doi": "10.1103/RevModPhys.71.S180", "primary_object": { "basename": "9808035.pdf", "url": "https://authors.library.caltech.edu/records/ee14h-j0v36/files/9808035.pdf" }, "related_objects": [ { "basename": "RevModPhys.71.S180.pdf", "url": "https://authors.library.caltech.edu/records/ee14h-j0v36/files/RevModPhys.71.S180.pdf" } ], "resource_type": "article", "pub_year": "1999", "author_list": "Horowitz, Gary T. and Teukolsky, Saul A." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/m14g0-zgj88", "eprint_id": 87489, "eprint_status": "archive", "datestamp": "2023-08-22 13:07:06", "lastmod": "2023-10-18 21:13:00", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Irrotational Binary Neutron Stars in Quasi-Equilibrium in General Relativity", "ispublished": "pub", "full_text_status": "public", "keywords": "binaries: close; gravitation; hydrodynamics; relativity; stars: neutron; stars: rotation", "note": "\u00a9 1998. The American Astronomical Society. \n\nReceived 1998 March 9; accepted 1998 April 7. \n\nI thank Larry Kidder for helpful discussions. This work was supported in part by NSF grant PHY 94-08378 to Cornell University, and by the Grand Challenge grant NSF PHY 93-18152/ASC 93-18152.\n\nPublished - Teukolsky_1998_ApJ_504_442.pdf
Submitted - 9803082.pdf
", "abstract": "Neutron stars in binary orbit emit gravitational waves and spiral slowly together. During this inspiral, they are expected to have very little vorticity. It is in fact a good approximation to treat the system as having zero vorticity, i.e., as irrotational. Because the orbital period is much shorter than the radiation reaction timescale, it is also an excellent approximation to treat the system as evolving through a sequence of equilibrium states, in each of which the gravitational radiation is neglected. In Newtonian gravity, one can simplify the hydrodynamic equations considerably for an equilibrium irrotational binary by introducing a velocity potential. The equations reduce to a Poisson-like equation for the potential, and a Bernoulli-type integral for the density. We show that a similar simplification can be carried out in general relativity. The resulting equations are much easier to solve than other formulations of the problem.", "date": "1998-09-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "504", "number": "1", "publisher": "American Astronomical Society", "pagerange": "442-449", "id_number": "CaltechAUTHORS:20180629-150439865", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180629-150439865", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY 94-08378" }, { "agency": "NSF", "grant_number": "PHY 93-18152" }, { "agency": "NSF", "grant_number": "ASC 93-18152" } ] }, "doi": "10.1086/306082", "primary_object": { "basename": "9803082.pdf", "url": "https://authors.library.caltech.edu/records/m14g0-zgj88/files/9803082.pdf" }, "related_objects": [ { "basename": "Teukolsky_1998_ApJ_504_442.pdf", "url": "https://authors.library.caltech.edu/records/m14g0-zgj88/files/Teukolsky_1998_ApJ_504_442.pdf" } ], "resource_type": "article", "pub_year": "1998", "author_list": "Teukolsky, Saul A." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/fmfbm-xcd98", "eprint_id": 87495, "eprint_status": "archive", "datestamp": "2023-08-19 03:14:35", "lastmod": "2023-10-18 21:13:16", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." } }, { "id": "Baumgarte-T-W", "name": { "family": "Baumgarte", "given": "Thomas W." } }, { "id": "Cook-G-B", "name": { "family": "Cook", "given": "Gregory B." } }, { "id": "Shapiro-S-L", "name": { "family": "Shapiro", "given": "Stuart L." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Treating instabilities in a hyperbolic formulation of Einstein's equations", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 1998 American Physical Society.\n\n(Received 15 September 1997; published 27 July 1998) \n\nWe thank Andrew Abrahams, \u00c9anna Flanagan, Pablo Laguna, and James York for helpful discussions. This work was supported by the NSF Binary Black Hole Grand Challenge Grants Nos. NSF PHY 93-18152 and ASC 93-18152 (ARPA supplemented), NSF Grant No. PHY 94-08378 at Cornell, and NSF Grant No. AST 96-18524 and NASA Grant No. NAG 5-3420 at Illinois. Some computations were performed on the Cornell Theory Center SP2 and on the National Center for Supercomputing Applications SGI Origin 2000.\n\nPublished - PhysRevD.58.044020.pdf
Accepted Version - 9807029
", "abstract": "We have recently constructed a numerical code that evolves a spherically symmetric spacetime using a hyperbolic formulation of Einstein's equations. For the case of a Schwarzschild black hole, this code works well at early times, but quickly becomes inaccurate on a time scale of 10-100 M, where M is the mass of the hole. We present an analytic method that facilitates the detection of instabilities. Using this method, we identify a term in the evolution equations that leads to a rapidly-growing mode in the solution. After eliminating this term from the evolution equations by means of algebraic constraints, we can achieve free evolution for times exceeding 10000M. We discuss the implications for three-dimensional simulations.", "date": "1998-08-15", "date_type": "published", "publication": "Physical Review D", "volume": "58", "number": "4", "publisher": "American Physical Society", "pagerange": "Art. No. 044020", "id_number": "CaltechAUTHORS:20180629-153601374", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180629-153601374", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY 93-18152" }, { "agency": "NSF", "grant_number": "ASC 93-18152" }, { "agency": "Advanced Research Projects Agency (ARPA)" }, { "agency": "NSF", "grant_number": "PHY 94-08378" }, { "agency": "NSF", "grant_number": "AST 96-18524" }, { "agency": "NASA", "grant_number": "NAG 5-3420" } ] }, "doi": "10.1103/PhysRevD.58.044020", "primary_object": { "basename": "PhysRevD.58.044020.pdf", "url": "https://authors.library.caltech.edu/records/fmfbm-xcd98/files/PhysRevD.58.044020.pdf" }, "related_objects": [ { "basename": "9807029", "url": "https://authors.library.caltech.edu/records/fmfbm-xcd98/files/9807029" } ], "resource_type": "article", "pub_year": "1998", "author_list": "Scheel, Mark A.; Baumgarte, Thomas W.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/9qwcn-nmg42", "eprint_id": 87491, "eprint_status": "archive", "datestamp": "2023-08-19 03:02:06", "lastmod": "2023-10-18 21:13:05", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Baumgarte-T-W", "name": { "family": "Baumgarte", "given": "T. W." } }, { "id": "Cook-G-B", "name": { "family": "Cook", "given": "G. B." } }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "M. A." } }, { "id": "Shapiro-S-L", "name": { "family": "Shapiro", "given": "S. L." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "S. A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "General relativistic models of binary neutron stars in quasiequilibrium", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 1998 American Physical Society. \n\n(Received 12 September 1997; published 8 May 1998) \n\nIt is a pleasure to thank Manish Parashar for his help with the implementation of DAGH and Andrew Abrahams, James Lombardi and Fred Rasio for several helpful discussions. We would also like to thank Matthew Duez, Eric Engelhard and John Fregeau for helping with the visualization of our data and the production of Fig. 1. This work was supported by NSF Grant AST 96-18524 and NASA Grant NAG 5-3420 at Illinois, NSF Grant PHY 94-08378 at Cornell, and by the NSF Binary Black Hole Grand Challenge Grants Nos. NSF PHY 93-18152 and ASC 93-18152 (ARPA supplemented). Computations were performed at the Cornell Center for Theory and Simulation in Science and Engineering and the National Center for Supercomputing Applications, University of Illinois at Urbana-Champaign.\n\nPublished - PhysRevD.57.7299.pdf
Submitted - 9709026
", "abstract": "We perform fully relativistic calculations of binary neutron stars in corotating, circular orbit. While Newtonian gravity allows for a strict equilibrium, a relativistic binary system emits gravitational radiation, causing the system to lose energy and slowly spiral inwards. However, since inspiral occurs on a time scale much longer than the orbital period, we can treat the binary to be in quasiequilibrium. In this approximation, we integrate a subset of the Einstein equations coupled to the relativistic equation of hydrostatic equilibrium to solve the initial value problem for binaries of arbitrary separation. We adopt a polytropic equation of state to determine the structure and maximum mass of neutron stars in close binaries for polytropic indices n = 1, 1.5 and 2. We construct sequences of constant rest-mass and locate turning points along energy equilibrium curves to identify the onset of orbital instability. In particular, we locate the innermost stable circular orbit and its angular velocity. We construct the first contact binary systems in full general relativity. These arise whenever the equation of state is sufficiently soft (n \u2273 1.5). A radial stability analysis reveals no tendency for neutron stars in close binaries to collapse to black holes prior to merger.", "date": "1998-06-15", "date_type": "published", "publication": "Physical Review D", "volume": "57", "number": "12", "publisher": "American Physical Society", "pagerange": "7299-7311", "id_number": "CaltechAUTHORS:20180629-151330543", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180629-151330543", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST 96-18524" }, { "agency": "NASA", "grant_number": "NAG 5-3420" }, { "agency": "NSF", "grant_number": "PHY 94-08378" }, { "agency": "NSF", "grant_number": "PHY 93-18152" }, { "agency": "NSF", "grant_number": "ASC 93-18152" }, { "agency": "Advanced Research Projects Agency (ARPA)" } ] }, "collection": "CaltechAUTHORS", "doi": "10.1103/PhysRevD.57.7299", "primary_object": { "basename": "9709026", "url": "https://authors.library.caltech.edu/records/9qwcn-nmg42/files/9709026" }, "related_objects": [ { "basename": "PhysRevD.57.7299.pdf", "url": "https://authors.library.caltech.edu/records/9qwcn-nmg42/files/PhysRevD.57.7299.pdf" } ], "resource_type": "article", "pub_year": "1998", "author_list": "Baumgarte, T. W.; Cook, G. B.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/bhr9h-xbt54", "eprint_id": 87496, "eprint_status": "archive", "datestamp": "2023-08-19 02:53:34", "lastmod": "2023-10-18 21:13:19", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Baumgarte-T-W", "name": { "family": "Baumgarte", "given": "T. W." } }, { "id": "Cook-G-B", "name": { "family": "Cook", "given": "G. B." } }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "M. A." } }, { "id": "Shapiro-S-L", "name": { "family": "Shapiro", "given": "S. L." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "S. A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Stability of relativistic neutron stars in binary orbit", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 1998 American Physical Society. \n\n(Received 12 May 1997; published 28 April 1998) \n\nThis work was supported by NSF Grant AST 96-18524 and NASA Grant NAG 5-3420 at Illinois, and NSF Grant PHY 94-08378 at Cornell.\n\nPublished - PhysRevD.57.6181.pdf
Submitted - 9705023.pdf
", "abstract": "We analyze the stability of relativistic, quasi-equilibrium binary neutron stars in synchronized circular orbit. We explore stability against radial collapse to black holes prior to merger, and against orbital plunge. We apply theorems based on turning points along uniformly rotating sequences of constant angular momentum and rest mass to locate the onset of secular instabilities. We find that inspiraling binary neutron stars are stable against radial collapse to black holes all the way down to the innermost stable circular orbit.", "date": "1998-05-15", "date_type": "published", "publication": "Physical Review D", "volume": "57", "number": "10", "publisher": "American Physical Society", "pagerange": "6181-6184", "id_number": "CaltechAUTHORS:20180629-154227533", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180629-154227533", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST 96-18524" }, { "agency": "NASA", "grant_number": "NAG 5-3420" }, { "agency": "NSF", "grant_number": "PHY 94-08378" } ] }, "doi": "10.1103/PhysRevD.57.6181", "primary_object": { "basename": "9705023.pdf", "url": "https://authors.library.caltech.edu/records/bhr9h-xbt54/files/9705023.pdf" }, "related_objects": [ { "basename": "PhysRevD.57.6181.pdf", "url": "https://authors.library.caltech.edu/records/bhr9h-xbt54/files/PhysRevD.57.6181.pdf" } ], "resource_type": "article", "pub_year": "1998", "author_list": "Baumgarte, T. W.; Cook, G. B.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/yk2n2-whd17", "eprint_id": 99177, "eprint_status": "archive", "datestamp": "2023-08-19 02:39:16", "lastmod": "2023-10-18 17:55:57", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Cook-G-B", "name": { "family": "Cook", "given": "G. B." } }, { "id": "Huq-M-F", "name": { "family": "Huq", "given": "M. F." } }, { "id": "Klasky-S-A", "name": { "family": "Klasky", "given": "S. A." } }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "M. A." } }, { "id": "Abrahams-A-B", "name": { "family": "Abrahams", "given": "A. M." } }, { "id": "Anderson-A", "name": { "family": "Anderson", "given": "A." } }, { "id": "Anninos-P", "name": { "family": "Anninos", "given": "P." } }, { "id": "Baumgarte-T-W", "name": { "family": "Baumgarte", "given": "T. W." } }, { "id": "Bishop-N-T", "name": { "family": "Bishop", "given": "N. T." } }, { "id": "Brandt-S-R", "name": { "family": "Brandt", "given": "S. R." } }, { "id": "Browne-J-C", "name": { "family": "Browne", "given": "J. C." } }, { "id": "Camarda-K", "name": { "family": "Camarda", "given": "K." } }, { "id": "Choptuik-M-W", "name": { "family": "Choptuik", "given": "M. W." } }, { "id": "Correll-R-R", "name": { "family": "Correll", "given": "R. R." } }, { "id": "Evans-C-R", "name": { "family": "Evans", "given": "C. R." } }, { "id": "Finn-L-S", "name": { "family": "Finn", "given": "L. S." } }, { "id": "Fox-G-C", "name": { "family": "Fox", "given": "G. C." } }, { "id": "G\u00f3mez-R", "name": { "family": "G\u00f3mez", "given": "R." } }, { "id": "Haupt-T", "name": { "family": "Haupt", "given": "T." } }, { "id": "Kidder-L-E", "name": { "family": "Kidder", "given": "L. E." }, "orcid": "0000-0001-5392-7342" }, { "id": "Laguna-P", "name": { "family": "Laguna", "given": "P." } }, { "id": "Landry-Walter", "name": { "family": "Landry", "given": "W." } }, { "id": "Lehner-L", "name": { "family": "Lehner", "given": "L." } }, { "id": "Lenaghan-J", "name": { "family": "Lenaghan", "given": "J." } }, { "id": "Marsa-R-L", "name": { "family": "Marsa", "given": "R. L." } }, { "id": "Masso-J", "name": { "family": "Masso", "given": "J." } }, { "id": "Matzner-R-A", "name": { "family": "Matzner", "given": "R. A." } }, { "id": "Mitra-S", "name": { "family": "Mitra", "given": "S." } }, { "id": "Papadopoulos-P", "name": { "family": "Papadopoulos", "given": "P." } }, { "id": "Parashar-M", "name": { "family": "Parashar", "given": "M." } }, { "id": "Rezzolla-L", "name": { "family": "Rezzolla", "given": "L." } }, { "id": "Rupright-M-E", "name": { "family": "Rupright", "given": "M. E." } }, { "id": "Saied-F", "name": { "family": "Saied", "given": "F." } }, { "id": "Saylor-P-E", "name": { "family": "Saylor", "given": "P. E." } }, { "id": "Seidel-E", "name": { "family": "Seidel", "given": "E." } }, { "id": "Shapiro-S-L", "name": { "family": "Shapiro", "given": "S. L." }, "orcid": "0000-0002-3263-7386" }, { "id": "Shoemaker-D", "name": { "family": "Shoemaker", "given": "D." } }, { "id": "Smarr-L", "name": { "family": "Smarr", "given": "L." } }, { "id": "Suen-W-M", "name": { "family": "Suen", "given": "W. M." } }, { "id": "Szil\u00e1gyi-B", "name": { "family": "Szil\u00e1gyi", "given": "B." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "S. A." }, "orcid": "0000-0001-9765-4526" }, { "id": "van-Putten-M-H-P-M", "name": { "family": "van Putten", "given": "M. H. P. M." } }, { "id": "Walker-P", "name": { "family": "Walker", "given": "P." } }, { "id": "Winicour-J", "name": { "family": "Winicour", "given": "J." } }, { "id": "York-J-W-Jr", "name": { "family": "York", "given": "J. W., Jr." } } ] }, "title": "Boosted Three-Dimensional Black-Hole Evolutions with Singularity Excision", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 1998 The American Physical Society. \n\nReceived 26 November 1997. \n\nThis work was supported by the NSF Binary Black Hole Grand Challenge Grants No. NSF PHY/ASC 93-18152 (ARPA supplemented), No. NSF PHY 93-10083, and Metacenter Grant No. MCA94P015N. Computations were performed at NPAC (Syracuse University), at NCSA (University of Illinois at Urbana-Champaign), and at the Pittsburgh Supercomputing Center.\n\nPublished - PhysRevLett.80.2512.pdf
Submitted - 9711078.pdf
", "abstract": "Binary black-hole interactions provide potentially the strongest source of gravitational radiation for detectors currently under development. We present some results from the Binary Black Hole Grand Challenge Alliance three-dimensional Cauchy evolution module. These constitute essential steps towards modeling such interactions and predicting gravitational radiation waveforms. We report on single black-hole evolutions and the first successful demonstration of a black hole moving freely through a three-dimensional computational grid via a Cauchy evolution: a hole moving near 6M at 0.1c during a total evolution of duration near 60M.", "date": "1998-03-23", "date_type": "published", "publication": "Physical Review Letters", "volume": "80", "number": "12", "publisher": "American Physical Society", "pagerange": "2512-2516", "id_number": "CaltechAUTHORS:20191009-084004889", "issn": "0031-9007", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20191009-084004889", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY/ASC 93-18152" }, { "agency": "NSF", "grant_number": "PHY 93-10083" }, { "agency": "Metacenter", "grant_number": "MCA94P015N" } ] }, "corp_creators": { "items": [ "Binary Black Hole Grand Challenge Alliance" ] }, "doi": "10.1103/physrevlett.80.2512", "primary_object": { "basename": "PhysRevLett.80.2512.pdf", "url": "https://authors.library.caltech.edu/records/yk2n2-whd17/files/PhysRevLett.80.2512.pdf" }, "related_objects": [ { "basename": "9711078.pdf", "url": "https://authors.library.caltech.edu/records/yk2n2-whd17/files/9711078.pdf" } ], "resource_type": "article", "pub_year": "1998", "author_list": "Cook, G. B.; Huq, M. F.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/ttjjg-qv278", "eprint_id": 88434, "eprint_status": "archive", "datestamp": "2023-08-19 02:36:11", "lastmod": "2023-10-18 22:03:29", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Abrahams-A-B", "name": { "family": "Abrahams", "given": "A. M." } }, { "id": "Rezzolla-L", "name": { "family": "Rezzolla", "given": "L." } }, { "id": "Rupright-M-E", "name": { "family": "Rupright", "given": "M. E." } }, { "id": "Anderson-A", "name": { "family": "Anderson", "given": "A." } }, { "id": "Anninos-P", "name": { "family": "Anninos", "given": "P." } }, { "id": "Baumgarte-T-W", "name": { "family": "Baumgarte", "given": "T. W." } }, { "id": "Bishop-N-T", "name": { "family": "Bishop", "given": "N. T." } }, { "id": "Brandt-S-R", "name": { "family": "Brandt", "given": "S. R." } }, { "id": "Browne-J-C", "name": { "family": "Browne", "given": "J. C." } }, { "id": "Camarda-K", "name": { "family": "Camarda", "given": "K." } }, { "id": "Choptuik-M-W", "name": { "family": "Choptuik", "given": "M. W." } }, { "id": "Cook-G-B", "name": { "family": "Cook", "given": "G. B." } }, { "id": "Correll-R-R", "name": { "family": "Correll", "given": "R. R." } }, { "id": "Evans-C-R", "name": { "family": "Evans", "given": "C. R." } }, { "id": "Finn-L-S", "name": { "family": "Finn", "given": "L. S." } }, { "id": "Fox-G-C", "name": { "family": "Fox", "given": "G. C." } }, { "id": "G\u00f3mez-R", "name": { "family": "G\u00f3mez", "given": "R." } }, { "id": "Haupt-T", "name": { "family": "Haupt", "given": "T." } }, { "id": "Huq-M-F", "name": { "family": "Huq", "given": "M. F." } }, { "id": "Kidder-L-E", "name": { "family": "Kidder", "given": "L. E." }, "orcid": "0000-0001-5392-7342" }, { "id": "Klasky-S-A", "name": { "family": "Klasky", "given": "S. A." } }, { "id": "Laguna-P", "name": { "family": "Laguna", "given": "P." } }, { "id": "Landry-Walter", "name": { "family": "Landry", "given": "W." } }, { "id": "Lehner-L", "name": { "family": "Lehner", "given": "L." } }, { "id": "Lenaghan-J", "name": { "family": "Lenaghan", "given": "J." } }, { "id": "Marsa-R-L", "name": { "family": "Marsa", "given": "R. L." } }, { "id": "Masso-J", "name": { "family": "Masso", "given": "J." } }, { "id": "Matzner-R-A", "name": { "family": "Matzner", "given": "R. A." } }, { "id": "Mitra-S", "name": { "family": "Mitra", "given": "S." } }, { "id": "Papadopoulos-P", "name": { "family": "Papadopoulos", "given": "P." } }, { "id": "Parashar-M", "name": { "family": "Parashar", "given": "M." } }, { "id": "Saied-F", "name": { "family": "Saied", "given": "F." } }, { "id": "Saylor-P-E", "name": { "family": "Saylor", "given": "P. E." } }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "M. A." } }, { "id": "Seidel-E", "name": { "family": "Seidel", "given": "E." } }, { "id": "Shapiro-S-L", "name": { "family": "Shapiro", "given": "S. L." } }, { "id": "Shoemaker-D", "name": { "family": "Shoemaker", "given": "D." } }, { "id": "Smarr-L", "name": { "family": "Smarr", "given": "L." } }, { "id": "Szil\u00e1gyi-B", "name": { "family": "Szil\u00e1gyi", "given": "B." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "S. A." }, "orcid": "0000-0001-9765-4526" }, { "id": "van-Putten-M-H-P-M", "name": { "family": "van Putten", "given": "M. H. P. M." } }, { "id": "Walker-P", "name": { "family": "Walker", "given": "P." } }, { "id": "Winicour-J", "name": { "family": "Winicour", "given": "J." } }, { "id": "York-J-W", "name": { "family": "York", "given": "J. W." } } ] }, "title": "Gravitational Wave Extraction and Outer Boundary Conditions by Perturbative Matching", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 1998 The American Physical Society. \n\nReceived 29 September 1997. \n\nThis work was supported by the NSF Binary Black Hole Grand Challenge Grants No. NSF PHY 93-18152, No. NSF PHY 93-10083, and No. ASC 93-18152 (ARPA supplemented). Computations were performed at NPAC (Syracuse University) and at NCSA (University of Illinois at Urbana-Champaign).\n\nPublished - PhysRevLett.80.1812.pdf
Submitted - 9709082.pdf
", "abstract": "We present a method for extracting gravitational radiation from a three-dimensional numerical relativity simulation and, using the extracted data, to provide outer boundary conditions. The method treats dynamical gravitational variables as nonspherical perturbations of Schwarzschild geometry. We discuss a code which implements this method and present results of tests which have been performed with a three-dimensional numerical relativity code.", "date": "1998-03-02", "date_type": "published", "publication": "Physical Review Letters", "volume": "80", "number": "9", "publisher": "American Physical Society", "pagerange": "1812-1815", "id_number": "CaltechAUTHORS:20180801-100851962", "issn": "0031-9007", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180801-100851962", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY 93-18152" }, { "agency": "NSF", "grant_number": "PHY 93-10083" }, { "agency": "NSF", "grant_number": "ASC 93-18152" }, { "agency": "Advanced Research Projects Agency (ARPA)" } ] }, "doi": "10.1103/physrevlett.80.1812", "primary_object": { "basename": "PhysRevLett.80.1812.pdf", "url": "https://authors.library.caltech.edu/records/ttjjg-qv278/files/PhysRevLett.80.1812.pdf" }, "related_objects": [ { "basename": "9709082.pdf", "url": "https://authors.library.caltech.edu/records/ttjjg-qv278/files/9709082.pdf" } ], "resource_type": "article", "pub_year": "1998", "author_list": "Abrahams, A. M.; Rezzolla, L.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/6sgh0-3nh05", "eprint_id": 87499, "eprint_status": "archive", "datestamp": "2023-08-19 02:25:05", "lastmod": "2023-10-18 21:13:26", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Rezzolla-L", "name": { "family": "Rezzolla", "given": "L." } }, { "id": "Abrahams-A-B", "name": { "family": "Abrahams", "given": "A. M." } }, { "id": "Baumgarte-T-W", "name": { "family": "Baumgarte", "given": "T. W." } }, { "id": "Cook-G-B", "name": { "family": "Cook", "given": "G. B." } }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "M. A." } }, { "id": "Shapiro-S-L", "name": { "family": "Shapiro", "given": "S. L." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "S. A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Waveform propagation in black hole spacetimes: Evaluating the quality of numerical solutions", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 1998 American Physical Society. \n\n(Received 21 August 1997; published 18 December 1997) \n\nThis work was supported by the NSF Binary Black Hole Grand Challenge Grant Nos. NSF PHY 93-18152/ASC 93-18152 (ARPA supplemented).\n\nPublished - PhysRevD.57.1084.pdf
Submitted - 9712037.pdf
", "abstract": "We compute the propagation and scattering of linear gravitational waves off a Schwarzschild black hole using a numerical code which solves a generalization of the Zerilli equation to a three-dimensional Cartesian coordinate system. Since the solution to this problem is well understood it represents a very good testbed for evaluating our ability to perform three-dimensional computations of gravitational waves in spacetimes in which a black hole event horizon is present.", "date": "1998-01-15", "date_type": "published", "publication": "Physical Review D", "volume": "57", "number": "2", "publisher": "American Physical Society", "pagerange": "1084-1091", "id_number": "CaltechAUTHORS:20180629-155501427", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180629-155501427", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY 93-18152" }, { "agency": "NSF", "grant_number": "ASC 93-18152" }, { "agency": "Advanced Research Projects Agency (ARPA)" } ] }, "doi": "10.1103/PhysRevD.57.1084", "primary_object": { "basename": "9712037.pdf", "url": "https://authors.library.caltech.edu/records/6sgh0-3nh05/files/9712037.pdf" }, "related_objects": [ { "basename": "PhysRevD.57.1084.pdf", "url": "https://authors.library.caltech.edu/records/6sgh0-3nh05/files/PhysRevD.57.1084.pdf" } ], "resource_type": "article", "pub_year": "1998", "author_list": "Rezzolla, L.; Abrahams, A. M.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/kr7jf-vpt73", "eprint_id": 87500, "eprint_status": "archive", "datestamp": "2023-08-19 02:02:34", "lastmod": "2023-10-18 21:13:28", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." } }, { "id": "Baumgarte-T-W", "name": { "family": "Baumgarte", "given": "Thomas W." } }, { "id": "Cook-G-B", "name": { "family": "Cook", "given": "Gregory B." } }, { "id": "Shapiro-S-L", "name": { "family": "Shapiro", "given": "Stuart L." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Numerical evolution of black holes with a hyperbolic formulation of general relativity", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 1997 American Physical Society. \n\n(Received 19 June 1997) \n\nWe thank Manish Parashar for his help with the DAGH system, and Andrew Abrahams, Charles Evans, Ed Seidel, Wai-Mo Suen, and James York for helpful discussions. This work was supported by the NSF Binary Black Hole Grand Challenge Grant No. NSF PHY 93-18152/ASC 93-18152 (ARPA supplemented), NSF Grant No. PHY 94-08378 at Cornell, and NSF Grant No. AST 96-18524 and NASA Grant No. NAG 5-3420 at Illinois.\n\nPublished - PhysRevD.56.6320.pdf
Submitted - 9708067.pdf
", "abstract": "We describe a numerical code that solves Einstein's equations for a Schwarzschild black hole in spherical symmetry, using a hyperbolic formulation introduced by Choquet-Bruhat and York. This is the first time this formulation has been used to evolve a numerical spacetime containing a black hole. We excise the hole from the computational grid in order to avoid the central singularity. We describe in detail a causal differencing method that should allow one to stably evolve a hyperbolic system of equations in three spatial dimensions with an arbitrary shift vector, to second-order accuracy in both space and time. We demonstrate the success of this method in the spherically symmetric case.", "date": "1997-11-15", "date_type": "published", "publication": "Physical Review D", "volume": "56", "number": "10", "publisher": "American Physical Society", "pagerange": "6320-6335", "id_number": "CaltechAUTHORS:20180629-155912237", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180629-155912237", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY 93-18152" }, { "agency": "NSF", "grant_number": "ASC 93-18152" }, { "agency": "Advanced Research Projects Agency (ARPA)" }, { "agency": "NSF", "grant_number": "PHY 94-08378" }, { "agency": "NSF", "grant_number": "AST 96-18524" }, { "agency": "NASA", "grant_number": "NAG 5-3420" } ] }, "collection": "CaltechAUTHORS", "doi": "10.1103/PhysRevD.56.6320", "primary_object": { "basename": "PhysRevD.56.6320.pdf", "url": "https://authors.library.caltech.edu/records/kr7jf-vpt73/files/PhysRevD.56.6320.pdf" }, "related_objects": [ { "basename": "9708067.pdf", "url": "https://authors.library.caltech.edu/records/kr7jf-vpt73/files/9708067.pdf" } ], "resource_type": "article", "pub_year": "1997", "author_list": "Scheel, Mark A.; Baumgarte, Thomas W.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/z9cwn-t8e81", "eprint_id": 88289, "eprint_status": "archive", "datestamp": "2023-08-19 01:47:42", "lastmod": "2023-10-18 21:56:40", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Press-W-H", "name": { "family": "Press", "given": "William H." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Numerical Recipes: Does This Paradigm Have a Future?", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 1997 AIP Publishing.\n\nPublished - 1.4822583.pdf
", "abstract": "Longtime readers of Computers in Physics may remember us as the editors/authors of the Numerical Recipes column that ran from 1988 through 1992. At that time, with the publication of the second edition of our Numerical Recipes (NR) books in C and Fortran, we took a sabbatical leave from column writing, a leave that became inadvertently permanent. Now, as a part of CIP's Tenth Anniversary celebration, we have been invited back to offer some observations about the past of scientific computing, including the educational niche occupied by our books, and to make some prognostications about where the field is going.", "date": "1997-09", "date_type": "published", "publication": "Computers in Physics", "volume": "11", "number": "5", "publisher": "American Institute of Physics", "pagerange": "416-424", "id_number": "CaltechAUTHORS:20180725-160852290", "issn": "0894-1866", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180725-160852290", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "doi": "10.1063/1.4822583", "primary_object": { "basename": "1.4822583.pdf", "url": "https://authors.library.caltech.edu/records/z9cwn-t8e81/files/1.4822583.pdf" }, "resource_type": "article", "pub_year": "1997", "author_list": "Press, William H. and Teukolsky, Saul A." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/exrz4-pcn84", "eprint_id": 87493, "eprint_status": "archive", "datestamp": "2023-08-19 01:44:09", "lastmod": "2023-10-18 21:13:11", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Baumgarte-T-W", "name": { "family": "Baumgarte", "given": "T. W." } }, { "id": "Cook-G-B", "name": { "family": "Cook", "given": "G. B." } }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "M. A." } }, { "id": "Shapiro-S-L", "name": { "family": "Shapiro", "given": "S. L." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "S. A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Binary Neutron Stars in General Relativity: Quasiequilibrium Models", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 1997 American Physical Society. \n\n(Received 8 April 1997) \n\nIt is a pleasure to thank Manish Parashar for his help with the implementation of DAGH, and Andrew Abrahams, James Lombardi, and Fred Rasio for several helpful discussions. This work was supported by NSF Grant AST 96-18524 and NASA Grant NAG 5-3420 at Illinois, NSF Grant PHY 94-08378 at Cornell, and by the NSF Binary Black Hole Grand Challenge Grant Nos. NSF PHY 93-18152/ASC 93-18152 (ARPA supplemented).\n\nPublished - PhysRevLett.79.1182.pdf
Submitted - 9704024.pdf
", "abstract": "We perform fully relativistic calculations of binary neutron stars in quasiequilibrium circular orbits. We integrate Einstein's equations together with the relativistic equation of hydrostatic equilibrium to solve the initial-value problem for equal-mass binaries of arbitrary separation. We construct sequences of constant rest mass and identify the innermost stable circular orbit and its angular velocity. We find that the quasiequilibrium maximum allowed mass of a neutron star in a close binary is slightly larger than in isolation.", "date": "1997-08-18", "date_type": "published", "publication": "Physical Review Letters", "volume": "79", "number": "7", "publisher": "American Physical Society", "pagerange": "1182-1185", "id_number": "CaltechAUTHORS:20180629-152837218", "issn": "0031-9007", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180629-152837218", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST 96-18524" }, { "agency": "NASA", "grant_number": "NAG 5-3420" }, { "agency": "NSF", "grant_number": "PHY 94-08378" }, { "agency": "NSF", "grant_number": "PHY 93-18152" }, { "agency": "NSF", "grant_number": "ASC 93-18152" }, { "agency": "Advanced Research Projects Agency (ARPA)" } ] }, "doi": "10.1103/PhysRevLett.79.1182", "primary_object": { "basename": "9704024.pdf", "url": "https://authors.library.caltech.edu/records/exrz4-pcn84/files/9704024.pdf" }, "related_objects": [ { "basename": "PhysRevLett.79.1182.pdf", "url": "https://authors.library.caltech.edu/records/exrz4-pcn84/files/PhysRevLett.79.1182.pdf" } ], "resource_type": "article", "pub_year": "1997", "author_list": "Baumgarte, T. W.; Cook, G. B.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/6eenm-r5s06", "eprint_id": 88290, "eprint_status": "archive", "datestamp": "2023-08-19 00:17:21", "lastmod": "2023-10-18 21:56:42", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "The explanation of the Trouton\u2013Noble experiment revisited", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 1996 American Association of Physics Teachers. \n\nI thank Kurt Gottfried for interesting me in this problem, and thank him and David Mermin for helpful discussions. This work was supported, in part, by the National Science Foundation.\n\nPublished - 1.18329.pdf
", "abstract": "One class of explanations of the null result of the Trouton\u2013Noble experiment uses the \"standard\" definitions of electromagnetic energy and momentum but is quite complicated. Another class is much simpler but appears to require new definitions of electromagnetic energy and momentum. We reconcile the two sets of explanations and show that they are both physically correct. We use the same arguments that have been used in discussions of the famous \"4/3\" factor in the electromagnetic mass of the classical electron.", "date": "1996-09", "date_type": "published", "publication": "American Journal of Physics", "volume": "64", "number": "9", "publisher": "American Association of Physics Teachers", "pagerange": "1104-1109", "id_number": "CaltechAUTHORS:20180725-160852372", "issn": "0002-9505", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180725-160852372", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF" } ] }, "doi": "10.1119/1.18329", "primary_object": { "basename": "1.18329.pdf", "url": "https://authors.library.caltech.edu/records/6eenm-r5s06/files/1.18329.pdf" }, "resource_type": "article", "pub_year": "1996", "author_list": "Teukolsky, Saul A." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/2ekhy-69116", "eprint_id": 87861, "eprint_status": "archive", "datestamp": "2023-08-18 23:53:34", "lastmod": "2023-10-18 21:29:42", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Baumgarte-T-W", "name": { "family": "Baumgarte", "given": "Thomas W." } }, { "id": "Cook-G-B", "name": { "family": "Cook", "given": "Gregory B." } }, { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." } }, { "id": "Shapiro-S-L", "name": { "family": "Shapiro", "given": "Stuart L." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Implementing an apparent-horizon finder in three dimensions", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 1996 American Physical Society. \n\n(Received 6 June 1996) \n\nWe would like to thank Peter Anninos and Edward Seidel for helpful discussions. This work was supported by NSF Grant Nos. AST 91-19475 and PHY 94-08378, NASA Grant No. NAG-2809, and by the Grand Challenge Grant Nos. NSF PHY 93-18152/ASC 93-18152 (ARPA supplemented). Computations were performed at the Cornell Center for Theory and Simulation in Science and Engineering, which is supported in part by the National Science Foundation, IBM Corporation, New York State, and the Cornell Research Institute.\n\nPublished - PhysRevD.54.4849.pdf
Submitted - 9606010.pdf
", "abstract": "Locating apparent horizons is not only important for a complete understanding of numerically generated spacetimes, but it may also be a crucial component of the technique for evolving black-hole spacetimes accurately. A scheme proposed by Libson, Mass\u00f3, Seidel, and Suen, based on expanding the location of the apparent horizon in terms of symmetric trace-free tensors, seems very promising for use with three-dimensional numerical data sets. In this paper, we generalize this scheme and perform a number of code tests to fully calibrate its behavior in black-hole spacetimes similar to those we expect to encounter in solving the binary black-hole coalescence problem. An important aspect of the generalization is that we can compute the symmetric trace-free tensor expansion to any order. This enables us to determine how far we must carry the expansion to achieve results of a desired accuracy. To accomplish this generalization, we describe a new and very convenient set of recurrence relations which apply to symmetric trace-free tensors.", "date": "1996-05-15", "date_type": "published", "publication": "Physical Review D", "volume": "54", "number": "8", "publisher": "American Physical Society", "pagerange": "4849-4857", "id_number": "CaltechAUTHORS:20180713-163543029", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180713-163543029", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST 91-19475" }, { "agency": "NSF", "grant_number": "PHY 94-08378" }, { "agency": "NASA", "grant_number": "NAG-2809" }, { "agency": "NSF", "grant_number": "PHY 93-18152" }, { "agency": "NSF", "grant_number": "ASC 93-18152" }, { "agency": "Advanced Research Projects Agency (ARPA)" } ] }, "doi": "10.1103/PhysRevD.54.4849", "primary_object": { "basename": "9606010.pdf", "url": "https://authors.library.caltech.edu/records/2ekhy-69116/files/9606010.pdf" }, "related_objects": [ { "basename": "PhysRevD.54.4849.pdf", "url": "https://authors.library.caltech.edu/records/2ekhy-69116/files/PhysRevD.54.4849.pdf" } ], "resource_type": "article", "pub_year": "1996", "author_list": "Baumgarte, Thomas W.; Cook, Gregory B.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/1wjdk-rey18", "eprint_id": 87862, "eprint_status": "archive", "datestamp": "2023-08-18 23:53:39", "lastmod": "2023-10-18 21:29:45", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Cook-G-B", "name": { "family": "Cook", "given": "Gregory B." } }, { "id": "Shapiro-S-L", "name": { "family": "Shapiro", "given": "Stuart L." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Testing a simplified version of Einstein's equations for numerical relativity", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 1996 American Physical Society. \n\n(Received 5 December 1995) \n\nWe thank E. Gourgoulhon for useful discussions about the work on relativistic virial quantities in Refs. [11,12]. This work was supported in part by NSF Grant Nos. AST 91- 19475 and PHY 94-08378, and by NASA Grant No. NAGW-2364 to Cornell University. We also acknowledge support from the Grand Challenge Grant No. NSF PHY 93-18152/ASC 93-18152.\n\nPublished - PhysRevD.53.5533.pdf
Submitted - 9512009.pdf
", "abstract": "Solving dynamical problems in general relativity requires the full machinery of numerical relativity. Wilson has proposed a simpler but approximate scheme for systems near equilibrium, such as binary neutron stars. We test the scheme on isolated, rapidly rotating, relativistic stars. Since these objects are in equilibrium, it is crucial that the approximation works well if we are to believe its predictions for more complicated systems such as binaries. Our results are very encouraging.", "date": "1996-05-15", "date_type": "published", "publication": "Physical Review D", "volume": "53", "number": "10", "publisher": "American Physical Society", "pagerange": "5533-5540", "id_number": "CaltechAUTHORS:20180713-164230222", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180713-164230222", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST 91-19475" }, { "agency": "NSF", "grant_number": "PHY 94-08378" }, { "agency": "NASA", "grant_number": "NAGW-2364" }, { "agency": "NSF", "grant_number": "PHY 93-18152" }, { "agency": "NSF", "grant_number": "ASC 93-18152" } ] }, "doi": "10.1103/PhysRevD.53.5533", "primary_object": { "basename": "9512009.pdf", "url": "https://authors.library.caltech.edu/records/1wjdk-rey18/files/9512009.pdf" }, "related_objects": [ { "basename": "PhysRevD.53.5533.pdf", "url": "https://authors.library.caltech.edu/records/1wjdk-rey18/files/PhysRevD.53.5533.pdf" } ], "resource_type": "article", "pub_year": "1996", "author_list": "Cook, Gregory B.; Shapiro, Stuart L.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/vfw6w-n3d63", "eprint_id": 87860, "eprint_status": "archive", "datestamp": "2023-08-20 06:51:34", "lastmod": "2023-10-18 21:29:40", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Shapiro-S-L", "name": { "family": "Shapiro", "given": "Stuart L." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" }, { "id": "Winicour-J", "name": { "family": "Winicour", "given": "Jeffrey" } } ] }, "title": "Toroidal black holes and topological censorship", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 1995 American Physical Society. \n\n(Received 21 July 1995) \n\nThis research was supported by NSF Grand Challenge Grant No. PHY93-18152/ASC93-18152 (ARPA supplemented). The work was also supported by NSF Grants Nos. PHY 92-08349 to the University of Pittsburgh and AST 91-19475 and PHY 94-08378 to Cornell University, as well as by NASA Grant No. NAG-2809 to Cornell. Computing resources were made available by the Pittsburgh Supercomputing Center and the Cornell Theory Center. We thank Ted Jacobson for interesting us in this problem.\n\nPublished - PhysRevD.52.6982.pdf
", "abstract": "Recent theorems regarding topological censorship are in apparent conflict with simulations of the collapse of rotating matter to form toroidal black holes. The geometry of a temporarily toroidal event horizon is analyzed and shown to be completely consistent with the theorems. A simple flat space model provides insight into the geometry of a toroidal black hole.", "date": "1995-12-15", "date_type": "published", "publication": "Physical Review D", "volume": "52", "number": "12", "publisher": "American Physical Society", "pagerange": "6982-6987", "id_number": "CaltechAUTHORS:20180713-163445285", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180713-163445285", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY 93-18152" }, { "agency": "NSF", "grant_number": "ASC 93-18152" }, { "agency": "Advanced Research Projects Agency (ARPA)" }, { "agency": "NSF", "grant_number": "PHY 92-08349" }, { "agency": "NSF", "grant_number": "AST 91-19475" }, { "agency": "NSF", "grant_number": "PHY 94-08378" }, { "agency": "NASA", "grant_number": "NAG-2809" } ] }, "doi": "10.1103/PhysRevD.52.6982", "primary_object": { "basename": "PhysRevD.52.6982.pdf", "url": "https://authors.library.caltech.edu/records/vfw6w-n3d63/files/PhysRevD.52.6982.pdf" }, "resource_type": "article", "pub_year": "1995", "author_list": "Shapiro, Stuart L.; Teukolsky, Saul A.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/mnc70-8zf31", "eprint_id": 88435, "eprint_status": "archive", "datestamp": "2023-09-15 05:59:30", "lastmod": "2023-10-23 21:22:35", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Matzner-R-A", "name": { "family": "Matzner", "given": "Richard A." } }, { "id": "Seidel-H-E", "name": { "family": "Seidel", "given": "H. E." } }, { "id": "Shapiro-S-L", "name": { "family": "Shapiro", "given": "Stuart L." } }, { "id": "Smarr-L", "name": { "family": "Smarr", "given": "L." } }, { "id": "Suen-W-M", "name": { "family": "Suen", "given": "W.-M." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" }, { "id": "Winicour-J", "name": { "family": "Winicour", "given": "J." } } ] }, "title": "Geometry of a Black Hole Collision", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 1995 American Association for the Advancement of Science. \n\nWe thank D. Eardley, R. Geroch, R. G\u00f3mez, J. M. Stewart, K. Thorne, F. Tipler, and M. Visser for helpful comments on this work. We are especially grateful to J. Mass\u00f3 and P. Walker for producing Fig. 10 and for contributing significantly to the analysis in this paper. We also thank M. Blanton, M. Chia, S. Hughes, C. Keeton, P. Walker, and K. Walsh for participating in the computation and production of Figs. 3 and 4. This research was funded by the NSF Grand Challenge Grant PHY93-18152/ASC93-18152 (ARPA supplemented) and supported by the following individual grants: by NSF grant PHY83 10083, Texas TARP-085, and a Cray University Research Grant (R.A.M.); by NCSA and by NSF grant PHY 94-07882 (H.E.S. and L.S.); by NSF grants AST 91-19475 and PHY 94-08378 and National Aeronautics and Space Administration grant NAGW-2364 (S.L.S. and S.A.T.); by NSF grant PHY 94-04788 (W.-M.S.); and by NSF grant PHY92-08349 (J.W.). Computer time was made available by NCSA and the Pittsburgh Supercomputing Center (in part through MetaCenter grant MCA94P015), and by the Cornell Center for Theory and Simulation in Science and Engineering (supported in part by NSF, IBM Corporation, New York State, and the Cornell Research Institute).\n\nPublished - 941.full.pdf
", "abstract": "The Binary Black Hole Alliance was formed to study the collision of black holes and the resulting gravitational radiation by computationally solving Einstein's equations for general relativity. The location of the black hole surface in a head-on collision has been determined in detail and is described here. The geometrical features that emerge are presented along with an analysis and explanation in terms of the spacetime curvature inherent in the strongly gravitating black hole region. This curvature plays a direct, important, and analytically explicable role in the formation and evolution of the event horizon associated with the surfaces of the black holes.", "date": "1995-11-10", "date_type": "published", "publication": "Science", "volume": "270", "number": "5238", "publisher": "American Association for the Advancement of Science", "pagerange": "941-947", "id_number": "CaltechAUTHORS:20180801-101749581", "issn": "0036-8075", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180801-101749581", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY 93-18152" }, { "agency": "NSF", "grant_number": "ASC 93-18152" }, { "agency": "NSF", "grant_number": "PHY 83-10083" }, { "agency": "Cray" }, { "agency": "National Center for Supercomputing Applications (NCSA)" }, { "agency": "NSF", "grant_number": "PHY 94-07882" }, { "agency": "NSF", "grant_number": "AST 91-19475" }, { "agency": "NSF", "grant_number": "PHY 94-08378" }, { "agency": "NASA", "grant_number": "NAGW-2364" }, { "agency": "NSF", "grant_number": "PHY 94-04788" }, { "agency": "NSF", "grant_number": "PHY 92-08349" }, { "agency": "Pittsburgh Supercomputing Center", "grant_number": "MCA94P015" }, { "agency": "Cornell Center for Theory and Simulation in Science and Engineering" }, { "agency": "Advanced Research Projects Agency (ARPA)" }, { "agency": "Texas Advanced Research Program", "grant_number": "TARP-085" } ] }, "doi": "10.1126/science.270.5238.941", "primary_object": { "basename": "941.full.pdf", "url": "https://authors.library.caltech.edu/records/mnc70-8zf31/files/941.full.pdf" }, "resource_type": "article", "pub_year": "1995", "author_list": "Matzner, Richard A.; Seidel, H. E.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/brn2z-4bs10", "eprint_id": 88424, "eprint_status": "archive", "datestamp": "2023-08-20 06:25:15", "lastmod": "2023-10-18 22:02:57", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Landry-Walter", "name": { "family": "Landry", "given": "Walter" } }, { "id": "Shapiro-S-L", "name": { "family": "Shapiro", "given": "Stuart L." }, "orcid": "0000-0002-3263-7386" }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Growth of perturbations in homogeneous collisionless collapse: discs versus spheres", "ispublished": "pub", "full_text_status": "public", "keywords": "instabilities - methods: numerical - galaxies: formation", "note": "\u00a9 1995 Royal Astronomical Society. Provided by the NASA Astrophysics Data System. \n\nAccepted 1995 April 26. Received 1995 March 7; in original form 1994 November 21. \n\nThis research was supported in part by NSF grants AST 91-19475 and PHY 94-08378 and NASA grant NAGW-2364 at Cornell University.\n\nPublished - 1995MNRAS_276__847L.pdf
", "abstract": "We study the growth of radial perturbations during the collapse of homogeneous spheres and discs. We model the sphere by concentric shells and the disc by concentric rings, initially at rest and allowed to move only radially. Our numerical experiments show only moderate growth in spheres but rapid growth in discs, leading to pronounced ring formation. For a sphere, the perturbations can be treated analytically as in cosmology. The growth rate is that of a power-law in time and independent of scale. For discs, we present an analytic solution for the perturbations using a suitable mode expansion. Shorter wavelength perturbations grow faster, exhibiting exponential growth at early times.", "date": "1995-10-01", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "276", "number": "3", "publisher": "Royal Astronomical Society", "pagerange": "847-858", "id_number": "CaltechAUTHORS:20180801-082944796", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180801-082944796", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST 91-19475" }, { "agency": "NSF", "grant_number": "PHY 94-08378" }, { "agency": "NASA", "grant_number": "NAGW-2364" } ] }, "doi": "10.1093/mnras/276.3.847", "primary_object": { "basename": "1995MNRAS_276__847L.pdf", "url": "https://authors.library.caltech.edu/records/brn2z-4bs10/files/1995MNRAS_276__847L.pdf" }, "resource_type": "article", "pub_year": "1995", "author_list": "Landry, Walter; Shapiro, Stuart L.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/ar894-rp011", "eprint_id": 88006, "eprint_status": "archive", "datestamp": "2023-08-20 05:43:58", "lastmod": "2023-10-18 21:35:56", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Abrahams-A-M", "name": { "family": "Abrahams", "given": "Andrew M." } }, { "id": "Shapiro-S-L", "name": { "family": "Shapiro", "given": "Stuart L." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Calculation of gravitational waveforms from black hole collisions and disk collapse: Applying perturbation theory to numerical spacetimes", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 1995 American Physical Society. \n\n(Received 26 August 1994) \n\nWe thank R. H. Price for stimulating conversations. This work was supported by National Science Foundation Grant Nos. AST 91-19475 and PHY 94-08378 and Grand Challenge Grant No. NSF PHY 93-18152/ACS 93-18152 (ARPA supplemented). Computations were performed at the Cornell Center for Theory and Simulation in Science and Engineering, which is supported in part by the National Science Foundation, IBM Corporation, New York State, and the Cornell Research Institute.\n\nPublished - PhysRevD.51.4295.pdf
Submitted - 9408036.pdf
", "abstract": "Many simulations of gravitational collapse to black holes become inaccurate before the total emitted gravitational radiation can be determined. The main difficulty is that a significant component of the radiation is still in the near-zone, strong field region at the time the simulation breaks down. We show how to calculate the emitted waveform by matching the numerical simulation to a perturbation solution when the final state of the system approaches a Schwarzschild black hole. We apply the technique to two scenarios: the head-on collision of two black holes and the collapse of a disk to a black hole. This is the first reasonably accurate calculation of the radiation generated from colliding black holes that form from matter collapse.", "date": "1995-04-15", "date_type": "published", "publication": "Physical Review D", "volume": "51", "number": "8", "publisher": "American Physical Society", "pagerange": "4295-4301", "id_number": "CaltechAUTHORS:20180719-133935208", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180719-133935208", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST 91-19475" }, { "agency": "NSF", "grant_number": "PHY 94-08378" }, { "agency": "NSF", "grant_number": "PHY 93-18152" }, { "agency": "Advanced Research Projects Agency (ARPA)" }, { "agency": "IBM" }, { "agency": "State of New York" }, { "agency": "Cornell Research Institute" } ] }, "doi": "10.1103/PhysRevD.51.4295", "primary_object": { "basename": "9408036.pdf", "url": "https://authors.library.caltech.edu/records/ar894-rp011/files/9408036.pdf" }, "related_objects": [ { "basename": "PhysRevD.51.4295.pdf", "url": "https://authors.library.caltech.edu/records/ar894-rp011/files/PhysRevD.51.4295.pdf" } ], "resource_type": "article", "pub_year": "1995", "author_list": "Abrahams, Andrew M.; Shapiro, Stuart L.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/tv1wv-w4c10", "eprint_id": 88008, "eprint_status": "archive", "datestamp": "2023-08-20 05:44:50", "lastmod": "2023-10-18 21:36:02", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." } }, { "id": "Shapiro-S-L", "name": { "family": "Shapiro", "given": "Stuart L." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Collapse to black holes in Brans-Dicke theory. I. Horizon boundary conditions for dynamical spacetimes", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 1995 American Physical Society. \n\n(Received 9 November 1994) \n\nWe would like to thank A. Abrahams and T. Baumgarte for helpful discussions. This work has been supported in part by National Science Foundation Grants No. AST 91-19475 and No. PHY 94-08378 and the Grand Challenge Grant No. NSF PHY 93-18152/ASC 93-18152 (ARPA supplemented) .\n\nPublished - PhysRevD.51.4208.pdf
Submitted - 9411025.pdf
", "abstract": "We present a new numerical code that evolves a spherically symmetric configuration of collisionless matter in the Brans-Dicke theory of gravitation. In this theory the spacetime is dynamical even in spherical symmetry, where it can contain gravitational radiation. Our code is capable of accurately tracking collapse to a black hole in a dynamical spacetime arbitrarily far into the future, without encountering either coordinate pathologies or spacetime singularities. This is accomplished by truncating the spacetime at a spherical surface inside the apparent horizon, and subsequently solving the evolution and constraint equations only in the exterior region. We use our code to address a number of long-standing theoretical questions about collapse to black holes in Brans-Dicke theory.", "date": "1995-04-15", "date_type": "published", "publication": "Physical Review D", "volume": "51", "number": "8", "publisher": "American Physical Society", "pagerange": "4208-4235", "id_number": "CaltechAUTHORS:20180719-135248763", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180719-135248763", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST 91-19475" }, { "agency": "NSF", "grant_number": "PHY 94-08378" }, { "agency": "NSF", "grant_number": "PHY 93-18152" }, { "agency": "Advanced Research Projects Agency (ARPA)" } ] }, "doi": "10.1103/PhysRevD.51.4208", "primary_object": { "basename": "9411025.pdf", "url": "https://authors.library.caltech.edu/records/tv1wv-w4c10/files/9411025.pdf" }, "related_objects": [ { "basename": "PhysRevD.51.4208.pdf", "url": "https://authors.library.caltech.edu/records/tv1wv-w4c10/files/PhysRevD.51.4208.pdf" } ], "resource_type": "article", "pub_year": "1995", "author_list": "Scheel, Mark A.; Shapiro, Stuart L.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/y5bw2-0n575", "eprint_id": 88007, "eprint_status": "archive", "datestamp": "2023-08-20 05:44:04", "lastmod": "2023-10-18 21:35:59", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." } }, { "id": "Shapiro-S-L", "name": { "family": "Shapiro", "given": "Stuart L." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Collapse to black holes in Brans-Dicke theory. II. Comparison with general relativity", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 1995 American Physical Society. \n\n(Received 9 November 1994) \n\nWe would like to thank T. Baumgarte for helpful discussions. This work has been supported in part by National Science Foundation Grants No. AST 91-19475 and No. PHY 94-08378 and the Grand Challenge Grant No. NSF PHY 93-18152/ASC 93-18152 (ARPA supplemented).\n\nPublished - PhysRevD.51.4236.pdf
Submitted - 9411026.pdf
", "abstract": "We discuss a number of long-standing theoretical questions about collapse to black holes in the Brans-Dicke theory of gravitation. Using a new numerical code we show that Oppenheimer-Snyder collapse in this theory produces black holes that are identical to those of general relativity in final equilibrium, but are quite different from those of general relativity during dynamical evolution. We find that there are epochs during which the apparent horizon of such a black hole passes outside the event horizon, and that the surface area of the event horizon decreases with time. This behavior is possible because theorems which prove otherwise assume R_(ab)l^al^b \u2265 0 for all null vectors l^a. We show that dynamical spacetimes in Brans-Dicke theory can violate this inequality, even in vacuum, for any value of \u03c9.", "date": "1995-04-15", "date_type": "published", "publication": "Physical Review D", "volume": "51", "number": "8", "publisher": "American Physical Society", "pagerange": "4236-4249", "id_number": "CaltechAUTHORS:20180719-134818063", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180719-134818063", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST 91-19475" }, { "agency": "NSF", "grant_number": "PHY 94-08378" }, { "agency": "NSF", "grant_number": "PHY 93-18152" }, { "agency": "Advanced Research Projects Agency (ARPA)" } ] }, "doi": "10.1103/PhysRevD.51.4236", "primary_object": { "basename": "9411026.pdf", "url": "https://authors.library.caltech.edu/records/y5bw2-0n575/files/9411026.pdf" }, "related_objects": [ { "basename": "PhysRevD.51.4236.pdf", "url": "https://authors.library.caltech.edu/records/y5bw2-0n575/files/PhysRevD.51.4236.pdf" } ], "resource_type": "article", "pub_year": "1995", "author_list": "Scheel, Mark A.; Shapiro, Stuart L.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/0nwhx-kh460", "eprint_id": 88018, "eprint_status": "archive", "datestamp": "2023-08-20 05:00:21", "lastmod": "2023-10-18 21:36:46", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Abrahams-A-M", "name": { "family": "Abrahams", "given": "Andrew M." } }, { "id": "Shapiro-S-L", "name": { "family": "Shapiro", "given": "Stuart L." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Disk collapse in general relativity", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 1994 American Physical Society. \n\n{Received 25 May 1994) \n\nThis work was supported by National Science Foundation Grant No. AST 91-19475 and No. PHY 90-07834 and by Grand Challenge Grant No. NSF PHY 93-18152/ASC 93-18152 (ARPA supplemented). Computations were performed at the Cornell Center for Theory and Simulation in Science and Engineering, which is supported in part by the National Science Foundation, IBM Corporation, New York State, and the Cornell Research Institute.\n\nPublished - PhysRevD.50.7282.pdf
Submitted - 9405060.pdf
", "abstract": "The radial collapse of a homogeneous disk of collisionless particles can be solved analytically in Newtonian gravitation. To solve the problem in general relativity, however, requires the full machinery of numerical relativity. The collapse of a disk is the simplest problem that exhibits the two most significant and challenging features of strong-field gravitation: black hole formation and gravitational wave generation. We carry out dynamical calculations of several different relativistic disk systems. We explore the growth of ring instabilities in equilibrium disks, and how they are suppressed by sufficient velocity dispersion. We calculate waveforms from oscillating disks, and from disks that undergo gravitational collapse to black holes. Studies of disk collapse to black holes should also be useful for developing new techniques for numerical relativity, such as apparent horizon boundary conditions for black hole spacetimes.", "date": "1994-12-15", "date_type": "published", "publication": "Physical Review D", "volume": "50", "number": "12", "publisher": "American Physical Society", "pagerange": "7282-7291", "id_number": "CaltechAUTHORS:20180719-144157648", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180719-144157648", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST 91-19475" }, { "agency": "NSF", "grant_number": "PHY 90-07834" }, { "agency": "NSF", "grant_number": "PHY 93-18152" }, { "agency": "Advanced Research Projects Agency (ARPA)" }, { "agency": "IBM" }, { "agency": "State of New York" }, { "agency": "Cornell Research Institute" } ] }, "doi": "10.1103/PhysRevD.50.7282", "primary_object": { "basename": "PhysRevD.50.7282.pdf", "url": "https://authors.library.caltech.edu/records/0nwhx-kh460/files/PhysRevD.50.7282.pdf" }, "related_objects": [ { "basename": "9405060.pdf", "url": "https://authors.library.caltech.edu/records/0nwhx-kh460/files/9405060.pdf" } ], "resource_type": "article", "pub_year": "1994", "author_list": "Abrahams, Andrew M.; Shapiro, Stuart L.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/zbaq1-y2z19", "eprint_id": 88019, "eprint_status": "archive", "datestamp": "2023-08-20 04:16:05", "lastmod": "2023-10-18 21:36:50", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Abrahams-A-M", "name": { "family": "Abrahams", "given": "Andrew M." } }, { "id": "Cook-G-B", "name": { "family": "Cook", "given": "Gregory B." } }, { "id": "Shapiro-S-L", "name": { "family": "Shapiro", "given": "Stuart L." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Solving Einstein's equations for rotating spacetimes: Evolution of relativistic star clusters", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 1994 American Physical Society. \n\n(Received 7 September 1993) \n\nThis work was supported by National Science Foundation Grants Nos. AST 91-19475 and PHY 90-07834. Computations were performed at the Cornell Center for Theory and Simulation in Science and Engineering, which is supported in part by the National Science Foundation, IBM Corporation, New York State, and the Cornell Research Institute.\n\nPublished - PhysRevD.49.5153.pdf
", "abstract": "A numerical relativity code designed to evolve rotating axisymmetric spacetimes is constructed. Both polarization states of gravitational radiation can be tracked. The source of the gravitational field is chosen to be a configuration of collisionless particles. The code is used to evaluate the stability of polytropic and toroidal star clusters. The formation of Kerr black holes by the collapse of unstable clusters is demonstrated. Unstable clusters with J/(M^2) < 1 collapse to black holes, while those with J/(M^2) > 1 collapse to new equilibrium configurations.", "date": "1994-05-15", "date_type": "published", "publication": "Physical Review D", "volume": "49", "number": "10", "publisher": "American Physical Society", "pagerange": "5153-5164", "id_number": "CaltechAUTHORS:20180719-144604603", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180719-144604603", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST 91-19475" }, { "agency": "NSF", "grant_number": "PHY 90-07834" }, { "agency": "IBM Corp." }, { "agency": "State of New York" }, { "agency": "Cornell Research Institute" } ] }, "doi": "10.1103/PhysRevD.49.5153", "primary_object": { "basename": "PhysRevD.49.5153.pdf", "url": "https://authors.library.caltech.edu/records/zbaq1-y2z19/files/PhysRevD.49.5153.pdf" }, "resource_type": "article", "pub_year": "1994", "author_list": "Abrahams, Andrew M.; Cook, Gregory B.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/8vks1-w8v73", "eprint_id": 88020, "eprint_status": "archive", "datestamp": "2023-08-20 04:10:31", "lastmod": "2023-10-18 21:36:54", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hughes-S-A", "name": { "family": "Hughes", "given": "Scott A." } }, { "id": "Keeton-C-R-II", "name": { "family": "Keeton", "given": "Charles R., II" } }, { "id": "Walker-P", "name": { "family": "Walker", "given": "Paul" } }, { "id": "Walsh-K-T", "name": { "family": "Walsh", "given": "Kevin T." } }, { "id": "Shapiro-S-L", "name": { "family": "Shapiro", "given": "Stuart L." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Finding black holes in numerical spacetimes", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 1994 American Physical Society. \n\n(Received 5 November 1993) \n\nWe thank Michael Blanton and Michael Chia for assistance with visualization and for help developing the horizon finder algorithm. We also thank Andrew Abrahams for useful discussions and Michael Piper for programming assistance in the early stages of the project. S.H., C.K, P.W., and K.W. were supported in part by the Research Experiences for Undergraduates program of the National Science Foundation. This research was supported in part by NSF Grants Nos. AST 91-19475 and PHY 90-07834 and NASA grant NAGW-2364 at Cornell University. Computations were performed at the Cornell Center for Theory and Simulation in Science and Engineering, which is supported in part by the National Science Foundation, IBM Corporation, New York State, and the Cornell Research Institute.\n\nPublished - PhysRevD.49.4004.pdf
", "abstract": "We have constructed a numerical code that finds black hole event horizons in an axisymmetric rotating spacetime. The spacetime is specified numerically by giving metric coefficients on a spatial grid for a series of time slices. The code solves the geodesic equation for light rays emitted from a suitable sample of points in the evolving spacetime. The algorithm for finding the event horizon employs the apparent horizon, which can form much later than the event horizon, to distinguish between light rays that escape to infinity and light rays that are captured. Simple geometries can be diagnosed on a workstation; more complicated cases are computationally intensive. However, the code is easily parallelized and has been efficiently run on the IBM SP-1 parallel machine. We have illustrated the use of the event horizon code on two cases. One is the head-on collision of two black holes that form from the collapse of collisionless matter, coalescing to a single Schwarzschild black hole. The other is the collapse of a rotating toroid to form a Kerr black hole. In this case the horizon initially appears with a toroidal topology. This is the first known example of this phenomenon.", "date": "1994-04-15", "date_type": "published", "publication": "Physical Review D", "volume": "49", "number": "8", "publisher": "American Physical Society", "pagerange": "4004-4015", "id_number": "CaltechAUTHORS:20180719-145058836", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180719-145058836", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST 91-19475" }, { "agency": "NSF", "grant_number": "PHY 90-07834" }, { "agency": "NASA", "grant_number": "NAGW-2364" }, { "agency": "IBM Corp." }, { "agency": "State of New York" }, { "agency": "Cornell Research Institute" } ] }, "doi": "10.1103/PhysRevD.49.4004", "primary_object": { "basename": "PhysRevD.49.4004.pdf", "url": "https://authors.library.caltech.edu/records/8vks1-w8v73/files/PhysRevD.49.4004.pdf" }, "resource_type": "article", "pub_year": "1994", "author_list": "Hughes, Scott A.; Keeton, Charles R., II; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/ham3k-kmw44", "eprint_id": 87497, "eprint_status": "archive", "datestamp": "2023-08-20 03:57:50", "lastmod": "2023-10-18 21:13:21", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Shapiro-S-L", "name": { "family": "Shapiro", "given": "Stuart L." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Scalar gravitation: A laboratory for numerical relativity. II. Disks", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 1994 American Physical Society. \n\n(Received 27 August 1993) \n\nWe thank M. Scheel for several useful discussions. This research was supported in part by NSF Grants AST 91-19475 and PHY 90-07834 and NASA Grant NAGW-2364 at Cornell University.\n\nPublished - PhysRevD.49.1886.pdf
", "abstract": "While not a correct physical theory, relativistic scalar gravitation provides a simple test site for developing many of the tools of numerical relativity. Using this theory, we have built a mean-field particle simulation scheme to study the dynamical behavior of collisionless disks. Disks are one-dimensional matter sources of two-dimensional gravitational fields. One-dimensional disk sources can be evolved without excessive computational resources and yet they are able to generate nonspherical gravitational waves. We find that we are able to calculate smooth and accurate wave forms from time-varying disks, despite the stochastic representation of the matter source terms caused by sampling with a finite number of particles. A similar scheme should provide accurate wave forms in general relativity, provided sufficient computer resources are used.", "date": "1994-02-15", "date_type": "published", "publication": "Physical Review D", "volume": "49", "number": "4", "publisher": "American Physical Society", "pagerange": "1886-1893", "id_number": "CaltechAUTHORS:20180629-154736545", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180629-154736545", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST 91-19475" }, { "agency": "NSF", "grant_number": "PHY 90-07834" }, { "agency": "NASA", "grant_number": "NAGW-2364" } ] }, "doi": "10.1103/PhysRevD.49.1886", "primary_object": { "basename": "PhysRevD.49.1886.pdf", "url": "https://authors.library.caltech.edu/records/ham3k-kmw44/files/PhysRevD.49.1886.pdf" }, "resource_type": "article", "pub_year": "1994", "author_list": "Shapiro, Stuart L. and Teukolsky, Saul A." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/aaf71-62329", "eprint_id": 87498, "eprint_status": "archive", "datestamp": "2023-08-20 03:57:55", "lastmod": "2023-10-18 21:13:23", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "Mark A." } }, { "id": "Shapiro-S-L", "name": { "family": "Shapiro", "given": "Stuart L." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Scalar gravitation: A laboratory for numerical relativity. III. Axisymmetry", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 1994 American Physical Society. \n\n(Received 15 September 1993) \n\nWe thank A. Abrahams for useful discussions. This research was supported in part by NSF Grants Nos. AST 91-19475 and PHY 90-07834 and NASA Grant No. NAGW-2364 at Cornell University. Computations were performed at the Cornell Center for Theory and Simulation in Science and Engineering, which is supported in part by the National Science Foundation, IBM Corporation, New York State, and the Cornell Research Institute.\n\nPublished - PhysRevD.49.1894.pdf
", "abstract": "We construct a two-dimensional axisymmetric mean-field particle simulation scheme that solves the equations of relativistic scalar gravitation coupled to collisionless matter. Although scalar gravitation theory disagrees with experiment, it is useful as a testing ground for numerical methods used to solve the equations of general relativity, particularly in the generation of gravitational waves. We discuss methods for extracting the gravitational wave amplitude from the field variables, as well as methods for imposing an accurate outgoing-wave boundary condition on the scalar field at a finite radius. We find that for continuous matter distributions, our code is able to calculate smooth and accurate gravitational wave forms, despite the stochastic representation of the matter source terms caused by sampling with a finite number of particles. A similar scheme should provide accurate wave forms in general relativity, provided sufficient computer resources are used.", "date": "1994-02-15", "date_type": "published", "publication": "Physical Review D", "volume": "49", "number": "4", "publisher": "American Physical Society", "pagerange": "1894-1905", "id_number": "CaltechAUTHORS:20180629-155106904", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180629-155106904", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST 91-19475" }, { "agency": "NSF", "grant_number": "PHY 90-07834" }, { "agency": "NASA", "grant_number": "NAGW-2364" }, { "agency": "IBM" }, { "agency": "State of New York" }, { "agency": "Cornell Research Institute" } ] }, "doi": "10.1103/PhysRevD.49.1894", "primary_object": { "basename": "PhysRevD.49.1894.pdf", "url": "https://authors.library.caltech.edu/records/aaf71-62329/files/PhysRevD.49.1894.pdf" }, "resource_type": "article", "pub_year": "1994", "author_list": "Scheel, Mark A.; Shapiro, Stuart L.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/n8bz5-33264", "eprint_id": 88021, "eprint_status": "archive", "datestamp": "2023-08-20 02:57:08", "lastmod": "2023-10-18 21:36:57", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Scheel-M-A", "name": { "family": "Scheel", "given": "M." } }, { "id": "Shapiro-S-L", "name": { "family": "Shapiro", "given": "S. L." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "S. A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Equilibrium and stability of relativistic cylindrical polytropes", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 1993 American Physical Society. \n\n(Received 30 November 1992) \n\nThis research was supported in part by NSF Grant Nos. AST 91-19475 and PHY 90-07834 and NASA Grant No. NAGW-2364 at Cornell University.\n\nPublished - PhysRevD.48.592.pdf
", "abstract": "We examine the structure and radial stability of infinitely long cylindrical polytropes in general relativity. We show that in contrast with spherical polytropes, all cylindrical polytropes are stable. Thus pressure regeneration is not decisive in determining the behavior of cylindrical systems. We discuss how the behavior of infinite cylinders is qualitatively different from that of finite, asymptotically flat configurations. We argue that the use of infinite cylinders to gain physical insight into the collapse of finite aspherical systems may be misleading. In particular, the ability of pressure and rotation to always halt the collapse of an infinite cylinder to a naked singularity may not carry over to finite systems.", "date": "1993-07-15", "date_type": "published", "publication": "Physical Review D", "volume": "48", "number": "2", "publisher": "American Physical Society", "pagerange": "592-606", "id_number": "CaltechAUTHORS:20180719-145630067", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180719-145630067", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST 91-19475" }, { "agency": "NSF", "grant_number": "PHY 90-07834" }, { "agency": "NASA", "grant_number": "NAGW-2364" } ] }, "doi": "10.1103/PhysRevD.48.592", "primary_object": { "basename": "PhysRevD.48.592.pdf", "url": "https://authors.library.caltech.edu/records/n8bz5-33264/files/PhysRevD.48.592.pdf" }, "resource_type": "article", "pub_year": "1993", "author_list": "Scheel, M.; Shapiro, S. L.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/7an8t-hbh65", "eprint_id": 88016, "eprint_status": "archive", "datestamp": "2023-08-20 02:23:29", "lastmod": "2023-10-18 21:36:38", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Shapiro-S-L", "name": { "family": "Shapiro", "given": "Stuart L." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Scalar gravitation: A laboratory for numerical relativity", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 1993 American Physical Society. \n\n(Received 9 October 1992) \n\nThis research was supported in part by NSF Grants Nos. AST 90 15451 and PHY 90 07834 and NASA Grant No. NAGW-2364 at Cornell University.\n\nPublished - PhysRevD.47.1529.pdf
", "abstract": "While not a correct physical theory, relativistic scalar gravitation provides a simple test site for developing many of the tools of numerical relativity. In contrast with general relativity, scalar gravitation allows gravitational waves to be generated in spherical symmetry. Hence one needs only one spatial dimension to try out methods of calculating wave emission and propagation. Using this theory, we have built a mean-field particle simulation scheme to study the dynamical behavior of collisionless matter in spherical symmetry. We find that we are able to calculate smooth and accurate wave forms, despite the stochastic representation of the matter source terms caused by sampling with a finite number of particles. A similar scheme should provide accurate wave forms in general relativity, provided sufficient computer resources are used.", "date": "1993-02-15", "date_type": "published", "publication": "Physical Review D", "volume": "47", "number": "4", "publisher": "American Physical Society", "pagerange": "1529-1540", "id_number": "CaltechAUTHORS:20180719-143417421", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180719-143417421", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST 90-15451" }, { "agency": "NSF", "grant_number": "PHY 90-07834" }, { "agency": "NASA", "grant_number": "NAGW-2364" } ] }, "doi": "10.1103/PhysRevD.47.1529", "primary_object": { "basename": "PhysRevD.47.1529.pdf", "url": "https://authors.library.caltech.edu/records/7an8t-hbh65/files/PhysRevD.47.1529.pdf" }, "resource_type": "article", "pub_year": "1993", "author_list": "Shapiro, Stuart L. and Teukolsky, Saul A." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/csh6r-8bb28", "eprint_id": 88396, "eprint_status": "archive", "datestamp": "2023-08-20 01:43:50", "lastmod": "2023-10-18 22:01:49", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Shapiro-S-L", "name": { "family": "Shapiro", "given": "Stuart L." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Black holes, star clusters, and naked singularities: numerical solution of Einstein's equations", "ispublished": "pub", "full_text_status": "restricted", "note": "\u00a9 1992 Royal Society.", "abstract": "We describe a new method for the numerical solution of Einstein's equations for the dynamical evolution of a collisionless gas of particles in general relativity. The gravitational field can be arbitrarily strong and particle velocities can approach the speed of light. The computational method uses the tools of numerical relativity and N-body particle simulation to follow the full nonlinear behaviour of these systems. Specifically, we solve the Vlasov equation in general relativity by particle simulation. The gravitational field is integrated by using the 3 + 1 formalism of Arnowitt, Deser and Misner. Physical applications include the stability of relativistic star clusters the binding energy criterion for stability, and the collapse of star clusters to black holes. Astrophysical issues addressed include the possible origin of quasars and active galactic nuclei via the collapse of dense star clusters to supermassive black holes. The method described here also provides a new tool for studying the cosmic censorship hypothesis and the possibility of naked singularities. The formation of a naked singularity during the collapse of a finite object would pose a serious difficulty for the theory of general relativity. The hoop conjecture suggests that this possibility will never happen provided the object is sufficiently compact (\u2264M) in all of its spatial dimensions. But what about the collapse of a long, non-rotating, prolate object to a thin spindle? Such collapse leads to a strong singularity in newtonian gravitation. Using our numerical code to evolve collisionless gas spheroids in full general relativity, we find that in all cases the spheroids collapse to singularities. When the spheroids are sufficiently compact the singularities are hidden inside black holes. However, when the spheroids are sufficiently large there are no apparent horizons. These results lend support to the hoop conjecture and appear to demonstrate that naked singularities can form in asymptotically flat space-times.", "date": "1992-09-15", "date_type": "published", "publication": "Philosophical transactions of the Royal Society of London. Series A: Mathematical and physical sciences", "volume": "340", "number": "1658", "publisher": "Royal Society", "pagerange": "365-390", "id_number": "CaltechAUTHORS:20180731-145243113", "issn": "0080-4614", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180731-145243113", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "doi": "10.1098/rsta.1992.0073", "resource_type": "article", "pub_year": "1992", "author_list": "Shapiro, Stuart L. and Teukolsky, Saul A." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/qpfvz-2nd03", "eprint_id": 88014, "eprint_status": "archive", "datestamp": "2023-08-20 01:43:42", "lastmod": "2023-10-18 21:36:29", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Abrahams-A-M", "name": { "family": "Abrahams", "given": "Andrew M." } }, { "id": "Heiderich-K-R", "name": { "family": "Heiderich", "given": "Karen R." } }, { "id": "Shapiro-S-L", "name": { "family": "Shapiro", "given": "Stuart L." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Vacuum initial data, singularities, and cosmic censorship", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 1992 American Physical Society. \n\n(Received 1 April 1992) \n\nWe acknowledge useful conversations with G. B. Cook, L. S. Finn, J. L. Friedman, and K. S. Thorne. This research was supported in part by NSF Grants Nos. AST 90-15451 and PHY 90-07834 and NASA Grant No. NAGW-2364 at Cornell University. A. A. was supported by the NSF Division of Advanced Scientific Computing. Computations in support of this work were performed at the Cornell National Supercomputing Facility, which is supported in part by the National Science Foundation, IBM Corporation, New York State, and the Cornell Research Institute.\n\nPublished - PhysRevD.46.2452.pdf
", "abstract": "The formation of a naked singularity in a vacuum, asymptotically flat spacetime would be a clear violation of cosmic censorship. We find initial value solutions to Einstein's field equations that may lead to this behavior. We construct two families of asymptotically flat, axisymmetric vaccum solutions at a moment of time symmetry. The limiting members of these families are singular. Our first family represents a linear string of Schwarzschild black holes. We study the divergence of the gravitational tidal field outside the holes as their number along the string is increased. Our second family consists of prolate Brill gravitational wave packets. We examine the tidal field strength as the characteristic width of the wave is reduced towards zero. In both cases we find that configurations can be constructed with arbitrarily large fields that are not clothed by apparent horizons. These configurations are characterized by long, prolate concentrations of mass energy. We analyze our results in the context of the hoop conjecture.", "date": "1992-09-15", "date_type": "published", "publication": "Physical Review D", "volume": "46", "number": "6", "publisher": "American Physical Society", "pagerange": "2452-2463", "id_number": "CaltechAUTHORS:20180719-142636714", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180719-142636714", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST 90-15451" }, { "agency": "NSF", "grant_number": "PHY 90-07834" }, { "agency": "NASA", "grant_number": "NAGW-2364" }, { "agency": "IBM Corp." }, { "agency": "State of New York" }, { "agency": "Cornell Research Institute" } ] }, "doi": "10.1103/PhysRevD.46.2452", "primary_object": { "basename": "PhysRevD.46.2452.pdf", "url": "https://authors.library.caltech.edu/records/qpfvz-2nd03/files/PhysRevD.46.2452.pdf" }, "resource_type": "article", "pub_year": "1992", "author_list": "Abrahams, Andrew M.; Heiderich, Karen R.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/hxz6q-zrm64", "eprint_id": 86869, "eprint_status": "archive", "datestamp": "2023-08-20 01:13:49", "lastmod": "2023-10-18 20:39:34", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Shapiro-S-L", "name": { "family": "Shapiro", "given": "Stuart L." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Collisions of relativistic clusters and the formation of black holes", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 1992 American Physical Society. \n\n(Received 30 October 1991) \n\nThis research was supported in part by NSF Grants Nos. AST 90-15451 and PHY 90-07834 and NASA Grant No. NAGW-2364 at Cornell University. Computations were performed on the Cornell National Supercomputer Facility.\n\nPublished - PhysRevD.45.2739.pdf
", "abstract": "We perform numerical simulations of head-on collisions of relativistic clusters. The cluster particles interact only gravitationally, and so satisfy the collisionless Boltzmann equation in general relativity. We construct and follow the evolution of three classes of initial configurations: spheres of particles at rest; spheres of particles boosted towards each other; and spheres of particles in circular orbits about their respective centers. In the first two cases, the spheres implode towards their centers and may form black holes before colliding. These scenarios thus can be used to study the head-on collision of two black holes. In the third case the clusters are initially in equilibrium and cannot implode. In this case collision from rest leads either to coalescence and virialization, or collapse to a black hole. This scenario is the collisionless analog of colliding neutron stars in relativistic hydrodynamics.", "date": "1992-04-15", "date_type": "published", "publication": "Physical Review D", "volume": "45", "number": "8", "publisher": "American Physical Society", "pagerange": "2739-2750", "id_number": "CaltechAUTHORS:20180606-163206765", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180606-163206765", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST 90-15451" }, { "agency": "NSF", "grant_number": "PHY 90-07834" }, { "agency": "NASA", "grant_number": "NAGW-2364" } ] }, "doi": "10.1103/PhysRevD.45.2739", "primary_object": { "basename": "PhysRevD.45.2739.pdf", "url": "https://authors.library.caltech.edu/records/hxz6q-zrm64/files/PhysRevD.45.2739.pdf" }, "resource_type": "article", "pub_year": "1992", "author_list": "Shapiro, Stuart L. and Teukolsky, Saul A." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/a6261-fy496", "eprint_id": 86870, "eprint_status": "archive", "datestamp": "2023-08-20 01:12:59", "lastmod": "2023-10-18 20:39:36", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Shapiro-S-L", "name": { "family": "Shapiro", "given": "Stuart L." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Equilibrium stellar systems with spindle singularities", "ispublished": "pub", "full_text_status": "public", "keywords": "celestial mechanics, stellar dynamics \u2014 galaxies: kinematics and dynamics \u2014 globular clusters : general \u2014 relativity", "note": "\u00a9 1992. The American Astronomical Society. \n\nReceived 1991 July 19; accepted 1991 September 26. \n\nThis work has been supported in part by National Science Foundation grants AST 90-15451 and PHY 90-07834, and NASA grant NAGW-2364 at Cornell University.\n\nPublished - 1992ApJ___388__287S.pdf
", "abstract": "We construct equilibrium sequences of axisymmetric Newtonian clusters that tend toward singular states.\nThe distribution functions are chosen to be of the form f=/(E, J_z). The numerical method then determines the density and gravitational potential self-consistently to satisfy Poisson's equation. For the prolate models, spindle singularities arise from the depletion of angular momentum near the symmetry axis. While the resulting density enhancement is confined to the region near the axis, the influence of the spindle extends much further out through its tidal gravitational field. Centrally condensed prolate clusters may contain strong-field regions even though the spindle mass is small and the mean cluster eccentricity is not extreme. While the calculations performed here are entirely Newtonian, the issue of singularities is an important topic in general relativity. Equilibrium solutions for relativistic star clusters can provide a testing ground for exploring this issue. The methods used in this paper for building nonspherical clusters can be extended to relativistic systems.", "date": "1992-04-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "388", "number": "1", "publisher": "American Astronomical Society", "pagerange": "287-300", "id_number": "CaltechAUTHORS:20180606-163526118", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180606-163526118", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST 90-15451" }, { "agency": "NSF", "grant_number": "PHY 90-07834" }, { "agency": "NASA", "grant_number": "NAGW-2364" } ] }, "doi": "10.1086/171152", "primary_object": { "basename": "1992ApJ___388__287S.pdf", "url": "https://authors.library.caltech.edu/records/a6261-fy496/files/1992ApJ___388__287S.pdf" }, "resource_type": "article", "pub_year": "1992", "author_list": "Shapiro, Stuart L. and Teukolsky, Saul A." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/r02w1-exg08", "eprint_id": 86871, "eprint_status": "archive", "datestamp": "2023-08-20 01:10:00", "lastmod": "2023-10-18 20:39:39", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Shapiro-S-L", "name": { "family": "Shapiro", "given": "Stuart L." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Gravitational collapse of rotating spheroids and the formation of naked singularities", "ispublished": "pub", "full_text_status": "public", "note": "\u00a91992 American Physical Society. \n\n(Received 26 September 1991) \n\nWe thank A. Abrahams, H. Apostalatos, and K. Thorne for stimulating discussions. This research was supported in part by NSF Grants Nos. AST 90-15451 and PHY 90-07834 and NASA Grant No. NAGW-2364 at Cornell University. Computations were performed on the Cornell National Supercomputer Facility.\n\nPublished - PhysRevD.45.2006.pdf
", "abstract": "We explore numerically the effect of rotation on the collapse of collisionless gas spheroids in full general relativity. The spheroids are initially prolate and consist of equal numbers of corotating and counterrotating particles. We have previously shown that in the absence of rotation the spheroids all collapse to spindle singularities. When the spheroids are sufficiently compact, the singularities are hidden inside black holes. However, when the spheroids are large enough, there are no apparent horizons. These nonrotating spheroids are strong candidates for naked singularities. Here our simulations suggest that rotation significantly modifies the evolution when it is sufficiently large. Imploding configurations with appreciable rotation ultimately collapse to black holes. However, for small enough angular momentum, our simulations cannot at present distinguish rotating from nonrotating collapse: spindle singularities appear to arise without apparent horizons. Hence it is possible that even spheroids with some angular momentum may form naked singularities.", "date": "1992-03-15", "date_type": "published", "publication": "Physical Review D", "volume": "45", "number": "6", "publisher": "American Physical Society", "pagerange": "2006-2012", "id_number": "CaltechAUTHORS:20180606-164006165", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180606-164006165", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST 90-15451" }, { "agency": "NSF", "grant_number": "PHY 90-07834" }, { "agency": "NASA", "grant_number": "NAGW-2364" } ] }, "doi": "10.1103/PhysRevD.45.2006", "primary_object": { "basename": "PhysRevD.45.2006.pdf", "url": "https://authors.library.caltech.edu/records/r02w1-exg08/files/PhysRevD.45.2006.pdf" }, "resource_type": "article", "pub_year": "1992", "author_list": "Shapiro, Stuart L. and Teukolsky, Saul A." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/cmk9s-n1w17", "eprint_id": 86874, "eprint_status": "archive", "datestamp": "2023-08-20 01:08:07", "lastmod": "2023-10-18 20:39:46", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Rasio-F-A", "name": { "family": "Rasio", "given": "F. A." }, "orcid": "0000-0002-7132-418X" }, { "id": "Shapiro-S-L", "name": { "family": "Shapiro", "given": "S. L." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "S. A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Formation of a 'planet' by rapid evaporation of a pulsar's companion", "ispublished": "pub", "full_text_status": "public", "keywords": "pulsars - stars: planetary systems", "note": "\u00a9 European Southern Observatory 1992. \n\nReceived December 24, 1991; accepted January 10, 1992. \n\nWe thank L. Bildsten for a useful conversation, A. Thoul for a critical reading of the manuscript, and I. Wasserman for comments. This work has been supported in part by NSF grants AST90-15451 and PHY90-07834, and NASA grant NAGW-2364 to Cornell University.\n\nPublished - 1992A+A___256L__35R.pdf
", "abstract": "A planet-size object in circular orbit around a pulsar could be formed as the result of rapid evaporation of a more massive binary companion by the pulsar's radiation.", "date": "1992-03", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "256", "number": "2", "publisher": "EDP Sciences", "pagerange": "L35-L37", "id_number": "CaltechAUTHORS:20180606-165035387", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180606-165035387", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST90-15451" }, { "agency": "NSF", "grant_number": "PHY90-07834" }, { "agency": "NASA", "grant_number": "NAGW-2364" } ] }, "primary_object": { "basename": "1992A+A___256L__35R.pdf", "url": "https://authors.library.caltech.edu/records/cmk9s-n1w17/files/1992A+A___256L__35R.pdf" }, "resource_type": "article", "pub_year": "1992", "author_list": "Rasio, F. A.; Shapiro, S. L.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/132ff-7r537", "eprint_id": 86876, "eprint_status": "archive", "datestamp": "2023-08-20 01:01:53", "lastmod": "2023-10-18 20:39:53", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Rasio-F-A", "name": { "family": "Rasio", "given": "F. A." }, "orcid": "0000-0002-7132-418X" }, { "id": "Nicholson-P-D", "name": { "family": "Nicholson", "given": "P. D." }, "orcid": "0000-0003-2275-4463" }, { "id": "Shapiro-S-L", "name": { "family": "Shapiro", "given": "S. L." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "S. A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "An observational test for the existence of a planetary system orbiting PSR1257 + 12", "ispublished": "pub", "full_text_status": "restricted", "note": "\u00a9 1992 Nature Publishing Group. \n\nWe thank A. Wolszczan for discussions and for communicating results before publication. We also thank J Lissauer for drawing our attention to the Hill's sphere constraint. This work has been supported in part by NSF and NASA grants to Cornell University.", "abstract": "FOLLOWING the first report of an object of planetary mass orbiting a pulsar, Wolszczan and Frail have now reported the even more surprising discovery of two planet-size companions in orbit around the nearby millisecond pulsar PSR1257+12. The orbital periods of the two planets are about 98 days and 67 days, very close to a 3:2 ratio. Here we point out that, because of this near commensurability, the mutual gravitational perturbations of the two planets should produce not only small secular changes, but also larger periodic changes in their orbital elements. In particular, we find that changes in the eccentricities and orbital periods should become measurable within a few years. Such a measurement would help determine the three masses in the system and the inclinations of the orbits. More importantly, a detection of these changes, if they accord with the theoretical predictions presented here, would provide irrefutable confirmation that the periodic residuals observed by Wolszczan and Frail are indeed caused by orbiting planets, rather than some other effect. For the single planet-size object previously reported1 around the pulsar PS R1829\u201310, there is no dynamical test analogous to the one proposed here to confirm the planetary interpretation.", "date": "1992-01-23", "date_type": "published", "publication": "Nature", "volume": "355", "number": "6358", "publisher": "Nature Publishing Group", "pagerange": "325-326", "id_number": "CaltechAUTHORS:20180606-165654476", "issn": "0028-0836", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180606-165654476", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF" }, { "agency": "NASA" } ] }, "doi": "10.1038/355325a0", "resource_type": "article", "pub_year": "1992", "author_list": "Rasio, F. A.; Nicholson, P. D.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/km6c2-dqv98", "eprint_id": 88004, "eprint_status": "archive", "datestamp": "2023-08-20 00:38:11", "lastmod": "2023-10-18 21:35:51", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Shapiro-S-L", "name": { "family": "Shapiro", "given": "Stuart L." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Numerical Calculations of Black Holes and Naked Singularities", "ispublished": "pub", "full_text_status": "restricted", "note": "\u00a9 1991 The New York Academy of Sciences. \n\nThis work was supported in part by National Foundation Grants AST 87\u201014475 and PHY 90\u201007834 at Cornell University. \n\nWe thank A. Abrahams, M. Choptuik, C. Evans, and L. S. Finn for helpful discussions. Computations were performed on the Cornell National Supercomputer Facility.", "abstract": "In the past 25 years, we have become more ambitious. We would like to solve nonspherical problems, in two and even three spatial dimensions. A new feature of nonspherical gravitational collapse is the production of gravitational waves. With the advent of large-scale gravitational wave detectors now likely, one of our goals is to be able to calculate reliably the spectrum of gravitational radiation from various astrophysical sources. How close are we to achieving this goal? What is the status of numerical calculations of black hole formation?", "date": "1991-12", "date_type": "published", "publication": "Annals of the New York Academy of Sciences", "volume": "647", "number": "1", "publisher": "New York Academy of Sciences", "pagerange": "158-163", "id_number": "CaltechAUTHORS:20180719-131656861", "issn": "0077-8923", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180719-131656861", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST 87\u201014475" }, { "agency": "NSF", "grant_number": "PHY 90\u201007834" } ] }, "doi": "10.1111/j.1749-6632.1991.tb32167.x", "resource_type": "article", "pub_year": "1991", "author_list": "Shapiro, Stuart L. and Teukolsky, Saul A." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/v9qq1-g7686", "eprint_id": 87494, "eprint_status": "archive", "datestamp": "2023-08-19 23:45:21", "lastmod": "2023-10-18 21:13:13", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Shapiro-S-L", "name": { "family": "Shapiro", "given": "Stuart L." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Formation of naked singularities: The violation of cosmic censorship", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 1991 American Physical Society. \n\n(Received 7 September 1990) \n\nThis research was supported in part by National Science Foundation Grants No. AST 87-14475 and No. PHY 90-07834 at Cornell University. Computations were performed on the Cornell National Supercomputer Facility. We thank A. Abrahams, M. Choptuik, C. Evans, and L. S. Finn for helpful discussions.\n\nPublished - PhysRevLett.66.994.pdf
", "abstract": "We use a new numerical code to evolve collisionless gas spheroids in full general relativity. In all cases the spheroids collapse to singularities. When the spheroids are sufficiently compact, the singularities are hidden inside black holes. However, when the spheriods are sufficiently large, there are no apparent horizons. These results lend support to the hoop conjecture and appear to demonstrate that naked singularities can form in asymptotically flat spacetimes.", "date": "1991-02-25", "date_type": "published", "publication": "Physical Review Letters", "volume": "66", "number": "8", "publisher": "American Physical Society", "pagerange": "994-997", "id_number": "CaltechAUTHORS:20180629-153305570", "issn": "0031-9007", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180629-153305570", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST 87-14475" }, { "agency": "NSF", "grant_number": "PHY 90-07834" } ] }, "doi": "10.1103/PhysRevLett.66.994", "primary_object": { "basename": "PhysRevLett.66.994.pdf", "url": "https://authors.library.caltech.edu/records/v9qq1-g7686/files/PhysRevLett.66.994.pdf" }, "resource_type": "article", "pub_year": "1991", "author_list": "Shapiro, Stuart L. and Teukolsky, Saul A." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/6n6s2-kcy90", "eprint_id": 88438, "eprint_status": "archive", "datestamp": "2023-08-19 23:38:28", "lastmod": "2023-10-18 22:03:36", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Rasio-F-A", "name": { "family": "Rasio", "given": "F. A." }, "orcid": "0000-0002-7132-418X" }, { "id": "Shapiro-S-L", "name": { "family": "Shapiro", "given": "S. L." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "S. A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Eclipse mechanisms for binary pulsars", "ispublished": "pub", "full_text_status": "public", "keywords": "pulsars - stars: binaries", "note": "\u00a9 1991 European Southern Observatory. Provided by the NASA Astrophysics Data System. \n\nReceived September 20, accepted October 10, 1990. \n\nWe thank A. Fruchter, A. Lyne and R. Manchester for discussing observations in progress, and M. Blaskiewicz, D. Chernoff, J. Cordes, J. Shaham and I. Wasserman for valuable conversations. This research was supported in part by NSF grants AST 87-14475 and PHY 9007834 to Cornell University.\n\nPublished - 1991A+A___241L__25R.pdf
", "abstract": "The parameters of the new eclipsing millisecond pulsar PSR 1744 - 24A in Terzan 5 are sufficiently different from those of PSR 1957 + 20 that very severe constraints can be put now on the theoretical models and formation scenarios of such systems. Most importantly, the eclipse cannot be caused by refractive effects (either total reflection or bending of the radio signal paths). Instead, they very likely are produced by an absorption mechanism, possibly combined with pulse-smearing effects. A model based on free-free absorption by the gas evaporated from the companion remains viable in spite of difficulties. Independent of the particular eclipse mechanism, the results of some preliminary dynamical calculations of the evaporative flow are discussed.", "date": "1991-01", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "241", "number": "1", "publisher": "EDP Sciences", "pagerange": "L25-L28", "id_number": "CaltechAUTHORS:20180801-104055676", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180801-104055676", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST 87-14475" }, { "agency": "NSF", "grant_number": "PHY-9007834" } ] }, "primary_object": { "basename": "1991A+A___241L__25R.pdf", "url": "https://authors.library.caltech.edu/records/6n6s2-kcy90/files/1991A+A___241L__25R.pdf" }, "resource_type": "article", "pub_year": "1991", "author_list": "Rasio, F. A.; Shapiro, S. L.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/jjsk3-14s05", "eprint_id": 86866, "eprint_status": "archive", "datestamp": "2023-08-23 16:51:57", "lastmod": "2023-10-18 20:39:27", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Press-W-H", "name": { "family": "Press", "given": "William H." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Fredholm and Volterra Integral Equations of the Second Kind", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 1990 AIP Publishing.\n\nPublished - 1.4822946.pdf
", "abstract": "Integral equations are often the best way to formulate physics problems. However, the typical physics student gets almost no training in integral equations, in contrast to differential equations, for example. Many physicists thus believe that numerical solution of integral equations must be an extremely arcane topic, since it is almost never dealt with in numerical analysis textbooks!", "date": "1990-09", "date_type": "published", "publication": "Computers in Physics", "volume": "4", "number": "5", "publisher": "American Institute of Physics", "pagerange": "554-557", "id_number": "CaltechAUTHORS:20180606-161910353", "issn": "0894-1866", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180606-161910353", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "doi": "10.1063/1.4822946", "primary_object": { "basename": "1.4822946.pdf", "url": "https://authors.library.caltech.edu/records/jjsk3-14s05/files/1.4822946.pdf" }, "resource_type": "article", "pub_year": "1990", "author_list": "Press, William H. and Teukolsky, Saul A." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/4xswa-d3b65", "eprint_id": 86867, "eprint_status": "archive", "datestamp": "2023-08-19 22:55:03", "lastmod": "2023-10-18 20:39:29", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Shapiro-S-L", "name": { "family": "Shapiro", "given": "Stuart L." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" }, { "id": "Nakamura-Takashi", "name": { "family": "Nakamura", "given": "Takashi" } } ] }, "title": "Spin-up of a rapidly rotating star by angular momentum loss", "ispublished": "pub", "full_text_status": "public", "keywords": "pulsars \u2014 stars: neutron \u2014 stars: rotation \u2014 stars: white dwarfs", "note": "\u00a9 1990. The American Astronomical Society. \n\nReceived 1990 March 16; accepted 1990 April 11. \n\nIt is a pleasure to thank R. H. Durisen and L. S. Finn for several helpful discussions. This work has been supported in part by National Science Foundation grants AST 87-14475, PHY 86-03284 and INT 88-15793 at Cornell University. This cooperative research project has been supported jointly by the NSF and JSPS under the US-Japan Cooperative Science Program. Fellowship support from the John Simon Guggenheim Memorial Foundation is gratefully acknowledged by S. L. S.\n\nPublished - 1990ApJ___357L__17S.pdf
", "abstract": "Can a rotating star spin up by radiating away its angular momentum? And if so, what can we infer about the properties of such a star? We show that the spin of a rapidly rotating star like a pulsar can indeed increase as it radiates away energy and angular momentum. For this to happen the adiabatic index governing the equation of state must be very close to 4/3 if the star is rotating uniformly. Otherwise the star must be rotating differentially.", "date": "1990-07-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "357", "number": "1", "publisher": "American Astronomical Society", "pagerange": "L17-L20", "id_number": "CaltechAUTHORS:20180606-162410693", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180606-162410693", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST 87-14475" }, { "agency": "NSF", "grant_number": "PHY 86-03284" }, { "agency": "NSF", "grant_number": "INT 88-15793" }, { "agency": "Japan Society for the Promotion of Science (JSPS)" }, { "agency": "John Simon Guggenheim Foundation" } ] }, "doi": "10.1086/185756", "primary_object": { "basename": "1990ApJ___357L__17S.pdf", "url": "https://authors.library.caltech.edu/records/4xswa-d3b65/files/1990ApJ___357L__17S.pdf" }, "resource_type": "article", "pub_year": "1990", "author_list": "Shapiro, Stuart L.; Teukolsky, Saul A.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/jkp4t-vda55", "eprint_id": 86868, "eprint_status": "archive", "datestamp": "2023-08-19 22:54:07", "lastmod": "2023-10-18 20:39:32", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Press-W-H", "name": { "family": "Press", "given": "William H." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Orthogonal Polynomials and Gaussian Quadrature with Nonclassical Weight Functions", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 1990 AIP Publishing.\n\nPublished - 1.4822929.pdf
", "abstract": "The subject of orthogonal polynomials crops up in a variety of different applications in both analytic and numerical work. Every different weight function (defined below) implies a different set of orthogonal polynomials. For the few most common, \"classical\" weight functions, the resulting polynomials are tabulated in standard references. In this column we will show you how to construct your own orthogonal polynomials when the weight functiol1 in your problem is not one of the classical forms. As an application, we will show how you can use a set of such orthogonal polynomials to carry out an otherwise intractable Gaussian quadrature.", "date": "1990-07", "date_type": "published", "publication": "Computers in Physics", "volume": "4", "number": "4", "publisher": "American Institute of Physics", "pagerange": "423-426", "id_number": "CaltechAUTHORS:20180606-162828492", "issn": "0894-1866", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180606-162828492", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "doi": "10.1063/1.4822929", "primary_object": { "basename": "1.4822929.pdf", "url": "https://authors.library.caltech.edu/records/jkp4t-vda55/files/1.4822929.pdf" }, "resource_type": "article", "pub_year": "1990", "author_list": "Press, William H. and Teukolsky, Saul A." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/6gefh-1xz91", "eprint_id": 86872, "eprint_status": "archive", "datestamp": "2023-08-19 22:44:58", "lastmod": "2023-10-18 20:39:41", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Press-W-H", "name": { "family": "Press", "given": "William H." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Hypergeometric Functions by Direct Path Integration", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 1990 AIP Publishing.\n\nPublished - 1.4822917.pdf
", "abstract": "The proverb, \"the longest way round is the shortest way home,\" dating from the 17th century, applies as well to present-day computer programming. The technique of choice in many real-life computations is not necessarily the most efficient or elegant one, but may instead be the one that is quick to program and easy to check.", "date": "1990-05", "date_type": "published", "publication": "Computers in Physics", "volume": "4", "number": "3", "publisher": "American Institute of Physics", "pagerange": "320-323", "id_number": "CaltechAUTHORS:20180606-164319293", "issn": "0894-1866", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180606-164319293", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "doi": "10.1063/1.4822917", "primary_object": { "basename": "1.4822917.pdf", "url": "https://authors.library.caltech.edu/records/6gefh-1xz91/files/1.4822917.pdf" }, "resource_type": "article", "pub_year": "1990", "author_list": "Press, William H. and Teukolsky, Saul A." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/0pw9h-1e733", "eprint_id": 86875, "eprint_status": "archive", "datestamp": "2023-08-19 22:21:39", "lastmod": "2023-10-18 20:39:48", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Press-W-H", "name": { "family": "Press", "given": "William H." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Elliptic Integrals", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 1990 AIP Publishing.\n\nPublished - 1.4822893.pdf
", "abstract": "[no abstract]", "date": "1990-01", "date_type": "published", "publication": "Computers in Physics", "volume": "4", "number": "1", "publisher": "American Institute of Physics", "pagerange": "92-96", "id_number": "CaltechAUTHORS:20180606-165439812", "issn": "0894-1866", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180606-165439812", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "doi": "10.1063/1.4822893", "primary_object": { "basename": "1.4822893.pdf", "url": "https://authors.library.caltech.edu/records/0pw9h-1e733/files/1.4822893.pdf" }, "resource_type": "article", "pub_year": "1990", "author_list": "Press, William H. and Teukolsky, Saul A." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/r1cjw-xz585", "eprint_id": 95268, "eprint_status": "archive", "datestamp": "2023-08-19 10:35:33", "lastmod": "2023-10-20 19:03:27", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Press-W-H", "name": { "family": "Press", "given": "William H." } }, { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "On formation of close binaries by two-body tidal capture", "ispublished": "pub", "full_text_status": "public", "keywords": "stars: binaries \u2014 stars: stellar dynamics", "note": "\u00a9 1977 The American Astronomical Society. Provided by the NASA Astrophysics Data System. \n\nSupported in part by the National Science Foundation [PHY 76-14852] at Harvard University, and [PHY 76-07297] at Cornell University; also by grant [GP-30799X] at Princeton University. \n\nAlfred P. Sloan Foundation Research Fellow.\n\nPublished - 1977ApJ___213__183P.pdf
", "abstract": "We calculate in detail the two-body tidal capture mechanism of Fabian, Pringle, and Rees: when two unbound stars have a close encounter, they may become bound by the energy that each deposits into nonradial oscillations of the other. After dimensional scalings are removed, the process depends only on a single dimensionless parameter, and on the dimensionless envelope structure of the stars. General formulae are derived; for definiteness, we apply them to the specific case of stars with an n = 3 polytropic structure. Capture cross sections as a function of velocity and capture rates for an isothermal distribution are given for the case of equal-mass stars; other cases can easily be computed from the formulae given.", "date": "1977-04-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "213", "publisher": "American Astronomical Society", "pagerange": "183-192", "id_number": "CaltechAUTHORS:20190506-153505082", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190506-153505082", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY 76-14852" }, { "agency": "NSF", "grant_number": "PHY 76-07297" }, { "agency": "NSF", "grant_number": "GP-30799X" }, { "agency": "Alfred P. Sloan Foundation" } ] }, "doi": "10.1086/155143", "primary_object": { "basename": "1977ApJ___213__183P.pdf", "url": "https://authors.library.caltech.edu/records/r1cjw-xz585/files/1977ApJ___213__183P.pdf" }, "resource_type": "article", "pub_year": "1977", "author_list": "Press, William H. and Teukolsky, Saul A." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/4hw5r-ef190", "eprint_id": 88198, "eprint_status": "archive", "datestamp": "2023-08-19 08:05:29", "lastmod": "2023-10-18 21:51:52", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Teukolsky-S-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526" } ] }, "title": "Rotating Black Holes: Separable Wave Equations for Gravitational and Electromagnetic Perturbations", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 1972 American Physical Society. \n\n(Received 10 July 1972) \n\nI thank William H. Press and Kip S. Thorne for helpful discussions.\n\nPublished - PhysRevLett.29.1114.pdf
", "abstract": "Separable wave equations with source terms are presented for electromagnetic and gravitational perturbations of an uncharged, rotating black hole. These equations describe the radiative field completely, and also part of the nonradiative field. Nontrivial, source-free, stationary perturbations are shown not to exist. The barrier integral governing synchrotron radiation from particles in circular orbits is shown to be the same as for scalar radiation. Future applications (stability of rotating black holes, \"spin-down,\" superradiant scattering, floating orbits) are outlined.", "date": "1972-10-16", "date_type": "published", "publication": "Physical Review Letters", "volume": "29", "number": "16", "publisher": "American Physical Society", "pagerange": "1114-1118", "id_number": "CaltechAUTHORS:20180724-143009027", "issn": "0031-9007", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180724-143009027", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "doi": "10.1103/physrevlett.29.1114", "primary_object": { "basename": "PhysRevLett.29.1114.pdf", "url": "https://authors.library.caltech.edu/records/4hw5r-ef190/files/PhysRevLett.29.1114.pdf" }, "resource_type": "article", "pub_year": "1972", "author_list": "Teukolsky, Saul A." } ]