[
{
"id": "thesis:17159",
"collection": "thesis",
"collection_id": "17159",
"cite_using_url": "https://resolver.caltech.edu/CaltechTHESIS:04162025-220303394",
"type": "thesis",
"title": "Numerical Modeling of High-energy Transients from Black Holes and Neutron Stars",
"author": [
{
"family_name": "Kim",
"given_name": "Yoonsoo",
"orcid": "0000-0002-4305-602",
"clpid": "Kim-Yoonsoo"
}
],
"thesis_advisor": [
{
"family_name": "Most",
"given_name": "Elias R.",
"orcid": "0000-0002-0491-1210",
"clpid": "Most-E-R"
},
{
"family_name": "Teukolsky",
"given_name": "Saul A.",
"orcid": "0000-0001-9765-4526",
"clpid": "Teukolsky-S-A"
}
],
"thesis_committee": [
{
"family_name": "Teukolsky",
"given_name": "Saul A.",
"orcid": "0000-0001-9765-4526",
"clpid": "Teukolsky-S-A"
},
{
"family_name": "Phinney",
"given_name": "E. Sterl",
"orcid": "0000-0002-9656-4032",
"clpid": "Phinney-E-S"
},
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Most",
"given_name": "Elias R.",
"orcid": "0000-0002-0491-1210",
"clpid": "Most-E-R"
}
],
"local_group": [
{
"literal": "div_pma"
}
],
"abstract": "Along with recent breakthroughs in relativistic astrophysics and multi-messenger astronomy, theoretical studies on compact objects and the dynamics of relativistic matter surrounding them have a growing significance. General relativistic approaches are required to properly describe astrophysical phenomena taking place in a strong gravity regime, yet the high complexity and nonlinearity of the equations governing those systems compel numerical approaches. In this thesis, we develop a computational method for and present global numerical simulations of relativistic plasma around compact objects, particularly focusing on high-energy electromagnetic transients originating from black holes and neutron stars. Our works include a new hybrid numerical scheme for modeling force-free magnetospheres of compact objects, large-scale simulations of a spinning black hole immersed in a magnetized wind, and magnetospheric transients from a merging black hole--neutron star binary.",
"doi": "10.7907/8skm-3x17",
"publication_date": "2025",
"thesis_type": "phd",
"thesis_year": "2025"
},
{
"id": "thesis:17301",
"collection": "thesis",
"collection_id": "17301",
"cite_using_url": "https://resolver.caltech.edu/CaltechTHESIS:05292025-212148506",
"type": "thesis",
"title": "An Electrodynamic Perspective of Black Holes",
"author": [
{
"family_name": "Boyeneni",
"given_name": "Siddharth",
"orcid": "0009-0000-7589-9602",
"clpid": "Boyeneni-Siddharth"
}
],
"thesis_advisor": [
{
"family_name": "Most",
"given_name": "Elias R.",
"orcid": "0000-0002-0491-1210",
"clpid": "Most-E-R"
}
],
"thesis_committee": [
{
"family_name": "None",
"given_name": "None"
}
],
"local_group": [
{
"literal": "TAPIR"
},
{
"literal": "div_pma"
}
],
"abstract": "Numerical relativity (NR) is a powerful modeling tool for the dynamics of general-relativistic systems that are difficult to analyze analytically. Prior work has led to a tetrad formulation of the 3+1 decomposition of the Einstein field equations (EFE) that bears a striking resemblance to electrodynamics, done by recasting Einstein\u2019s equations into a set of coupled nonlinear Maxwell equations. We use gravitational electric and magnetic fields developed from this theory to analytically probe Schwarzschild and Kerr solutions to the EFE. We compare the resulting Kerr dynamics with a numerical simulation of the Kerr spacetime. We then extend this analysis to visualize the inspiral, merger, and ring-down of a binary black hole collision simulated in moving puncture gauge.",
"doi": "10.7907/ypb6-3e47",
"publication_date": "2025",
"thesis_type": "senior_major",
"thesis_year": "2025"
},
{
"id": "thesis:17372",
"collection": "thesis",
"collection_id": "17372",
"cite_using_url": "https://resolver.caltech.edu/CaltechTHESIS:06022025-193721130",
"primary_object_url": {
"basename": "habib_sarah_2025.pdf",
"content": "final",
"filesize": 1447710,
"license": "other",
"mime_type": "application/pdf",
"url": "/17372/1/habib_sarah_2025.pdf",
"version": "v6.0.0"
},
"type": "thesis",
"title": "Error Quantification and Mitigation for Numerical Compact Binary Waveforms",
"author": [
{
"family_name": "Habib",
"given_name": "Sarah Mary",
"orcid": "0000-0002-4725-4978",
"clpid": "Habib-Sarah-Mary"
}
],
"thesis_advisor": [
{
"family_name": "Teukolsky",
"given_name": "Saul A.",
"orcid": "0000-0001-9765-4526",
"clpid": "Teukolsky-S-A"
},
{
"family_name": "Scheel",
"given_name": "Mark",
"orcid": "0000-0001-6656-9134",
"clpid": "Scheel-M-A"
},
{
"family_name": "Most",
"given_name": "Elias R.",
"orcid": "0000-0002-0491-1210",
"clpid": "Most-E-R"
}
],
"thesis_committee": [
{
"family_name": "Most",
"given_name": "Elias R.",
"orcid": "0000-0002-0491-1210",
"clpid": "Most-E-R"
},
{
"family_name": "Teukolsky",
"given_name": "Saul A.",
"orcid": "0000-0001-9765-4526",
"clpid": "Teukolsky-S-A"
},
{
"family_name": "Scheel",
"given_name": "Mark",
"orcid": "0000-0001-6656-9134",
"clpid": "Scheel-M-A"
},
{
"family_name": "Weinstein",
"given_name": "Alan Jay",
"orcid": "0000-0002-0928-6784",
"clpid": "Weinstein-Alan-J-Physics"
},
{
"family_name": "Chatziioannou",
"given_name": "Katerina",
"orcid": "0000-0002-5833-413X",
"clpid": "Chatziioannou-K"
},
{
"family_name": "Chen",
"given_name": "Yanbei",
"orcid": "0000-0002-9730-9463",
"clpid": "Chen-Yanbei"
}
],
"local_group": [
{
"literal": "div_pma"
}
],
"abstract": "Gravitational wave analysis requires waveform models to compare with observed signals from compact binaries. These models are based on and validated by numerical relativity waveforms---waveforms output from codes developed to numerically evolve the Einstein field equations. The efficacy of numerical waveforms for analysis is limited by error from both numerical and astrophysical sources. This thesis makes two contributions to the quantification and mitigation of this error.
\r\n\r\nChapter 2 describes a new algorithm for eccentricity reduction, the process of determining initial conditions for quasicircular binary orbits. This iterative procedure requires a measurement of eccentricity based on an early-inspiral trajectory. We find that the use of nonlinear fitting techniques such as variable projection leads to vastly improved consistency in eccentricity measurements.
\r\n\r\nFinally, Chapter 3 presents an in-depth quantification of error in numerical binary neutron star waveforms from three vastly different numerical relativity codes. We find that overall these codes produce consistent binary neutron star evolutions, but that further accuracy improvements will be required for analysis of next-generation gravitational wave detector signals.
",
"doi": "10.7907/jbre-7e68",
"publication_date": "2025",
"thesis_type": "phd",
"thesis_year": "2025"
}
]