[ { "id": "authors:x7hq2-t6996", "collection": "authors", "collection_id": "x7hq2-t6996", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:ADErmp98", "type": "article", "title": "Solar fusion cross sections", "author": [ { "family_name": "Adelberger", "given_name": "Eric G.", "clpid": "Adelberger-E-G" }, { "family_name": "Austin", "given_name": "Sam M.", "clpid": "Austin-S-M" }, { "family_name": "Bahcall", "given_name": "John N.", "clpid": "Bahcall-J-N" }, { "family_name": "Balantekin", "given_name": "A. B.", "clpid": "Balantekin-A-B" }, { "family_name": "Bogaert", "given_name": "Gilles", "clpid": "Bogaert-G" }, { "family_name": "Brown", "given_name": "Lowell S.", "clpid": "Brown-L-S" }, { "family_name": "Buchmann", "given_name": "Lothar", "clpid": "Buchmann-L" }, { "family_name": "Cecil", "given_name": "F. Edward", "clpid": "Cecil-F-E" }, { "family_name": "Champagne", "given_name": "Arthur E.", "clpid": "Champagne-A-E" }, { "family_name": "Braeckeleer", "given_name": "Ludwig de", "clpid": "Braeckeleer-L-D" }, { "family_name": "Duba", "given_name": "Charles A.", "clpid": "Elliott-C-A" }, { "family_name": "Elliott", "given_name": "Steven R.", "clpid": "Elliott\u00ad-S-R" }, { "family_name": "Freedman", "given_name": "Stuart J.", "clpid": "Freedman-S-J" }, { "family_name": "Gai", "given_name": "Moshe", "clpid": "Gai-M" }, { "family_name": "Goldring", "given_name": "G.", "clpid": "Goldring-G" }, { "family_name": "Gould", "given_name": "Christopher R.", "clpid": "Gould-C-R" }, { "family_name": "Gruzinov", "given_name": "Andrei", "clpid": "Gruzinov-A" }, { "family_name": "Haxton", "given_name": "Wick C.", "clpid": "Haxton-W-C" }, { "family_name": "Heeger", "given_name": "Karsten M.", "clpid": "Heeger-K-M" }, { "family_name": "Henley", "given_name": "Ernest", "clpid": "Henley-E" }, { "family_name": "Johnson", "given_name": "Calvin W.", "clpid": "Johnson-C-W" }, { "family_name": "Kamionkowski", "given_name": "Marc", "orcid": "0000-0001-7018-2055", "clpid": "Kamionkowski-M" }, { "family_name": "Kavanagh", "given_name": "Ralph W.", "clpid": "Kavanagh-R-W" }, { "family_name": "Koonin", "given_name": "Steven E.", "clpid": "Koonin-S-E" }, { "family_name": "Kubodera", "given_name": "Kuniharu", "clpid": "Kubodera-K" }, { "family_name": "Langanke", "given_name": "Karlheinz", "clpid": "Langanke-K" }, { "family_name": "Motobayashi", "given_name": "Tohru", "clpid": "Motobayashi-T" }, { "family_name": "Pandharipande", "given_name": "Vijay", "clpid": "Pandharipande-V" }, { "family_name": "Parker", "given_name": "Peter", "clpid": "Parker-P" }, { "family_name": "Robertson", "given_name": "R. G. H.", "clpid": "Robertson-R-G-H" }, { "family_name": "Rolfs", "given_name": "Claus", "clpid": "Rolfs-C" }, { "family_name": "Sawyer", "given_name": "R. F.", "clpid": "Sawyer-R-F" }, { "family_name": "Shaviv", "given_name": "N.", "clpid": "Shaviv-N" }, { "family_name": "Shoppa", "given_name": "T. D.", "clpid": "Shoppa-T-D" }, { "family_name": "Snover", "given_name": "K. A.", "clpid": "Snover-K-A" }, { "family_name": "Swanson", "given_name": "Erik", "clpid": "Swanson-E" }, { "family_name": "Tribble", "given_name": "Robert E.", "clpid": "Tribble-R-E" }, { "family_name": "Turck-Chi\u00e8ze", "given_name": "Sylvaine", "clpid": "Turck-Chi\u00e8ze-S" }, { "family_name": "Wilkerson", "given_name": "John F.", "clpid": "Wilkerson-J-F" } ], "abstract": "We review and analyze the available information on the nuclear-fusion cross sections that are most important for solar energy generation and solar neutrino production. We provide best values for the low-energy cross-section factors and, wherever possible, estimates of the uncertainties. We also describe the most important experiments and calculations that are required in order to improve our knowledge of solar fusion rates.", "doi": "10.1103/RevModPhys.70.1265", "issn": "0034-6861", "publisher": "American Physical Society", "publication": "Reviews of Modern Physics", "publication_date": "1998-10", "series_number": "4", "volume": "70", "issue": "4", "pages": "1265-1291" }, { "id": "authors:06xrm-1nv07", "collection": "authors", "collection_id": "06xrm-1nv07", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:BAHprc98a", "type": "article", "title": "Electron-screening correction for the proton-proton reaction", "author": [ { "family_name": "Bahcall", "given_name": "John N.", "clpid": "Bahcall-J-N" }, { "family_name": "Chen", "given_name": "Xuelei", "clpid": "Chen-Xuelei" }, { "family_name": "Kamionkowski", "given_name": "Marc", "orcid": "0000-0001-7018-2055", "clpid": "Kamionkowski-M" } ], "abstract": "We test the Salpeter formalism for the electron screening of the solar proton-proton fusion reaction by solving numerically the relevant Schr\u00f6dinger equation. We evaluate exactly the square of the overlap integral of the two-proton wave function and the deuteron wave function and compare with the usual analytic approximation. The usual WKB solution agrees with the numerical result to O(10^-4). The WKB approximation should be even more precise for the other nuclear fusion reactions in the pp chain and CNO cycles.", "doi": "10.1103/PhysRevC.57.2756", "issn": "0556-2813", "publisher": "American Physical Society", "publication": "Physical Review C", "publication_date": "1998-05", "series_number": "5", "volume": "57", "issue": "5", "pages": "2756-2759" }, { "id": "authors:kcnws-py273", "collection": "authors", "collection_id": "kcnws-py273", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:BAHrmp95", "type": "article", "title": "Solar models with helium and heavy-element diffusion", "author": [ { "family_name": "Bahcall", "given_name": "John N.", "clpid": "Bahcall-J-N" }, { "family_name": "Pinsonneault", "given_name": "M. H.", "orcid": "0000-0002-7549-7766", "clpid": "Pinsonneault-M-H" }, { "family_name": "Wasserburg", "given_name": "G. J.", "orcid": "0000-0002-7957-8029", "clpid": "Wasserburg-G-J" } ], "abstract": "Helium and heavy-element diffusion are both included in precise calculations of solar models. In addition, improvements in the input data for solar interior models are described for nuclear reaction rates, the solar luminosity, the solar age, heavy-element abundances, radiative opacities, helium and metal diffusion rates, and neutrino interaction cross sections. The effects on the neutrino fluxes of each change in the input physics are evaluated separately by constructing a series of solar models with one additional improvement added at each stage. The effective 1 \u03c3 uncertainties in the individual input quantities are estimated and used to evaluate the uncertainties in the calculated neutrino fluxes and the calculated event rates for solar neutrino experiments. The calculated neutrino event rates, including all of the improvements, are 9.3-1.4+1.2 SNU for the 37Cl experiment and 137-7+8 SNU for the 71Ga experiments. The calculated flux of 7Be neutrinos is 5.1 (1.00-0.07+0.06)\u00d710^9 cm^-2 s^-1 and the flux of 8B neutrinos is 6.6(1.00-0.17+0.14)\u00d710^6 cm^-2 s^-1. The primordial helium abundance found for this model is Y=0.278. The present-day surface abundance of the model is Ys=0.247, in agreement with the helioseismological measurement of Ys=0.242\u00b10.003 determined by Hernandez and Christensen-Dalsgaard (1994). The computed depth of the convective zone is R=0.712R\u2299, in agreement with the observed value determined from p-mode oscillation data of R=0.713\u00b10.003R\u2299 found by Christensen-Dalsgaard et al. (1991). Although the present results increase the predicted event rate in the four operating solar neutrino experiments by almost 1 \u03c3 (theoretical uncertainty), they only slightly increase the difficulty of explaining the existing experiments with standard physics (i.e., by assuming that nothing happens to the neutrinos after they are created in the center of the sun). For an extreme model in which all diffusion (helium and heavy-element diffusion) is neglected, the event rates are 7.0-1.0+0.9 SNU for the 37Cl experiment and 126-6+6 SNU for the 71Ga experiments, while the 7Be and 8B neutrino fluxes are, respectively, 4.5(1.00-0.07+0.06)\u00d710^9 cm^-2 s^-1 and 4.9(1.00-0.17+0.14)\u00d710^6 cm^-2 s^-1. For the no-diffusion model, the computed value of the depth of the convective zone is R=0.726R\u2299, which disagrees with the observed helioseismological value. The calculated surface abundance of helium, Ys=0.268, is also in disagreement with the p-mode measurement. The authors conclude that helioseismology provides strong evidence for element diffusion and therefore for the somewhat larger solar neutrino event rates calculated in this paper.", "doi": "10.1103/RevModPhys.67.781", "issn": "0034-6861", "publisher": "Reviews of Modern Physics", "publication": "Reviews of Modern Physics", "publication_date": "1995-10", "series_number": "4", "volume": "67", "issue": "4", "pages": "781-808" }, { "id": "authors:7fdmp-kck22", "collection": "authors", "collection_id": "7fdmp-kck22", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:BAHprd95a", "type": "article", "title": "Solar neutrinos: Radiative corrections in neutrino-electron scattering experiments", "author": [ { "family_name": "Bahcall", "given_name": "John N.", "clpid": "Bahcall-J-N" }, { "family_name": "Kamionkowski", "given_name": "Marc", "orcid": "0000-0001-7018-2055", "clpid": "Kamionkowski-M" }, { "family_name": "Sirlin", "given_name": "Alberto", "clpid": "Sirlin-A" } ], "abstract": "Radiative corrections to the electron recoil-energy spectra and to total cross sections are computed for neutrino-electron scattering by solid neutrinos. Radiative corrections change monotonically the electron recoil spectrum for incident 8B neutrinos, with the relative probability of observing recoil electrons being reduced by about 4% at the highest electron energies. For p-p and 7Be neutrinos, the recoil spectra are not affected significantly. Total cross sections for solar neutrino-electron scattering are reduced by about 2% compared to previously computed values. We also calculate the recoil spectra from 13N and 15O neutrinos including radiative corrections.", "doi": "10.1103/PhysRevD.51.6146", "issn": "2470-0010", "publisher": "American Physical Society", "publication": "Physical Review D", "publication_date": "1995-06-01", "series_number": "11", "volume": "51", "issue": "11", "pages": "6146-6158" }, { "id": "authors:2h0wv-3ss63", "collection": "authors", "collection_id": "2h0wv-3ss63", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:KAMprc94", "type": "article", "title": "Vacuum-polarization corrections to solar-fusion rates", "author": [ { "family_name": "Kamionkowski", "given_name": "Marc", "orcid": "0000-0001-7018-2055", "clpid": "Kamionkowski-M" }, { "family_name": "Bahcall", "given_name": "John N.", "clpid": "Bahcall-J-N" } ], "abstract": "The vacuum-polarization (VP) corrections to rates for nuclear-fusion reactions in the pp chain and in the CNO cycle are calculated. For the reactions of particular importance to the solar-neutrino problem, the 3He(3He,2p)4He, 3He(\u03b1,\u03b3)7Be, 7Be(p,\u03b3)8B, and 14N(p,\u03b3)15O reactions, we find the magnitude of the effect to be less than 2%. The effect of VP on all the other reaction rates is expected to be of a similar order of magnitude. We discuss how these results affect the predicted fluxes of solar neutrinos.", "doi": "10.1103/PhysRevC.49.545", "issn": "0556-2813", "publisher": "American Physical Society", "publication": "Physical Review C", "publication_date": "1994-01", "series_number": "1", "volume": "49", "issue": "1", "pages": "545-547" }, { "id": "authors:3tz4c-xwa87", "collection": "authors", "collection_id": "3tz4c-xwa87", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190529-103834433", "type": "article", "title": "A Search for High-Excitation Redshift Systems in the Absorption Spectra of Five Quasars", "author": [ { "family_name": "Bahcall", "given_name": "J. N.", "clpid": "Bahcall-J-N" }, { "family_name": "Joss", "given_name": "P. C.", "clpid": "Joss-P-C" }, { "family_name": "Cohen", "given_name": "J. G.", "orcid": "0000-0002-8039-4673", "clpid": "Cohen-J-G" } ], "abstract": "We have searched the absorption spectra of five quasars for the presence of redshift system dominated by the highly ionized doublets C iv, N v, and O vi, which could be the strongest lines produced by absorbing clouds with collisional ionization temperatures between 10^5 \u00b0 and 10^6 \u00b0K. There is at most marginal evidence for one such system apiece in the spectra of PHL 957 and 4C 05.34, which are the two quasars with the largest known emission redshifts. Highly ionized redshift systems of this type are not widespread among the five quasars we investigated; the number of redshifts found in the observed spectra is not significantly larger than the number found in similar random-number spectra. Less than 5 percent of the observed absorption lines are identified in a statistically significant way by redshift systems of this type.", "doi": "10.1086/152303", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "1973-08-15", "volume": "184", "pages": "57-63" }, { "id": "authors:dykwe-5qm83", "collection": "authors", "collection_id": "dykwe-5qm83", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170303-104227786", "type": "article", "title": "Optical and Near-Infrared Observations of the Nearby Spiral Galaxy Maffei 2", "author": [ { "family_name": "Spinrad", "given_name": "Hyron", "clpid": "Spinrad-H" }, { "family_name": "Bahcall", "given_name": "J.", "clpid": "Bahcall-J-N" }, { "family_name": "Becklin", "given_name": "E. E.", "clpid": "Becklin-E-E" }, { "family_name": "Gunn", "given_name": "James E.", "clpid": "Gunn-J-E" }, { "family_name": "Kristian", "given_name": "J.", "clpid": "Kristian-J" }, { "family_name": "Neugebauer", "given_name": "G.", "clpid": "Neugebauer-G" }, { "family_name": "Sargent", "given_name": "W. L. W.", "clpid": "Sargent-W-L-W" }, { "family_name": "Smith", "given_name": "H.", "clpid": "Smith-H" } ], "abstract": "Spectra, photographs, and photometric measurements have been used to show that Maffei 2 has a distance of 5 \u00b1 2 Mpc and that it has a morphological type near Sbc II-in agreement with similar conclusions made earlier by radio observers. We discuss the possible relationships between Maffei 2 and the elliptical galaxy Maffei 1; there are serious inconsistencies in the existing data which bear on this question.", "doi": "10.1086/151967", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "1973-03-01", "volume": "180", "pages": "351-358" }, { "id": "authors:nw6gc-1aa76", "collection": "authors", "collection_id": "nw6gc-1aa76", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:BAHprl71", "type": "article", "title": "Upper limit on neutrino energy associated with Weber pulses", "author": [ { "family_name": "Bahcall", "given_name": "John N.", "clpid": "Bahcall-J-N" }, { "family_name": "Davis", "given_name": "Raymond, Jr.", "clpid": "Davis-R-Jr" } ], "abstract": "An upper limit is established on the fraction of energy associated with the gravitational pulses reported by Weber that could be in the form of neutrinos with energies between 0.9 and 100 MeV.", "doi": "10.1103/PhysRevLett.26.662", "issn": "0031-9007", "publisher": "American Physical Society", "publication": "Physical Review Letters", "publication_date": "1971-03-15", "series_number": "11", "volume": "26", "issue": "11", "pages": "662-663" }, { "id": "authors:f8fxa-ccv30", "collection": "authors", "collection_id": "f8fxa-ccv30", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:BAHprl69", "type": "article", "title": "What next with solar neutrinos?", "author": [ { "family_name": "Bahcall", "given_name": "John N.", "clpid": "Bahcall-J-N" } ], "abstract": "The capture rate of solar neutrinos is estimated for a number of targets that have been suggested previously as possible detectors of solar neutrinos. It is shown that the most important feasible experiment to be carried out in the future employs 7Li as a detector.", "doi": "10.1103/PhysRevLett.23.251", "issn": "0031-9007", "publisher": "American Physical Society", "publication": "Physical Review Letters", "publication_date": "1969-08-04", "series_number": "5", "volume": "23", "issue": "5", "pages": "251-254" }, { "id": "authors:94yv9-nf575", "collection": "authors", "collection_id": "94yv9-nf575", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120815-093355459", "type": "article", "title": "Present Status of the Theoretical Predictions for the ^(37)Cl Solar-Neutrino Experiment", "author": [ { "family_name": "Bahcall", "given_name": "John N.", "clpid": "Bahcall-J-N" }, { "family_name": "Bahcall", "given_name": "Neta A.", "clpid": "Bahcall-N-A" }, { "family_name": "Shaviv", "given_name": "Giora", "clpid": "Shaviv-G" } ], "abstract": "The theoretical predictions for the ^(37)Cl solar-neutrino experiment are summarized and compared with the experimental results of Davis, Harmer, and Hoffman. Three important conclusions about the sun are shown to follow.", "doi": "10.1103/PhysRevLett.20.1209", "issn": "0031-9007", "publisher": "American Physical Society", "publication": "Physical Review Letters", "publication_date": "1968-05-20", "series_number": "21", "volume": "20", "issue": "21", "pages": "1209-1212" }, { "id": "authors:6534m-htt58", "collection": "authors", "collection_id": "6534m-htt58", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:BAHprl67", "type": "article", "title": "Does the fine-structure constant vary with cosmic time?", "author": [ { "family_name": "Bahcall", "given_name": "John N.", "clpid": "Bahcall-J-N" }, { "family_name": "Schmidt", "given_name": "Maarten", "clpid": "Schmidt-Maarten" } ], "abstract": "The fine structure constant at red shifts \u0394\u03bb / \u03bb\u22480.2, corresponding to an epoch around two billion years ago, has been determined using the wavelengths of a pair of O III emission lines measured in the spectra of five radio galaxies. We find \u03b1(z=0.2) / \u03b1(lab)=1.001\u00b10.002 probable error.", "doi": "10.1103/PhysRevLett.19.1294", "issn": "0031-9007", "publisher": "American Physical Society", "publication": "Physical Review Letters", "publication_date": "1967-11-27", "series_number": "22", "volume": "19", "issue": "22", "pages": "1294-1295" }, { "id": "authors:t253b-9vn28", "collection": "authors", "collection_id": "t253b-9vn28", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:BAHprl66", "type": "article", "title": "Solar neutrinos", "author": [ { "family_name": "Bahcall", "given_name": "John N.", "clpid": "Bahcall-J-N" } ], "abstract": "The predicted capture rate in the Cl37 experiment for detecting solar neutrinos is calculated using the results of recent nuclear experiments and solar-model investigations. It is shown that additional experiments (e.g., with H2, Li7, B11, or \u03bd-e scattering) are necessary to establish the relative contributions of the proton-proton chain and the CNO cycle to solar energy generation.", "doi": "10.1103/PhysRevLett.17.398", "issn": "0031-9007", "publisher": "American Physical Society", "publication": "Physical Review Letters", "publication_date": "1966-08-15", "series_number": "7", "volume": "17", "issue": "7", "pages": "398-401" }, { "id": "authors:fgkke-95c85", "collection": "authors", "collection_id": "fgkke-95c85", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:BAHpr65a", "type": "article", "title": "Neutron Stars. I. Properties at Absolute Zero Temperature", "author": [ { "family_name": "Bahcall", "given_name": "John N.", "clpid": "Bahcall-J-N" }, { "family_name": "Wolf", "given_name": "Richard A.", "orcid": "0000-0001-5291-4275", "clpid": "Wolf-Richard-A" } ], "abstract": "The properties of a neutron star at absolute zero temperature are discussed. The problem of determining the ground state of a neutron star is formulated in a general way and the conditions are described under which one might reasonably hope that an individual-particle model (which we adopt) is valid. The effects of the strong interactions on the number densities and production thresholds of the various hadrons are illustrated with several examples. The modification of the energy spectrum of neutrons and protons in a neutron star is calculated using an effective-mass approximation adapted from the theory of nuclear matter. Crude estimates are made of the contributions of hadrons other than nucleons to the equation of state and specific heat.", "doi": "10.1103/PhysRev.140.B1445", "issn": "0031-899X", "publisher": "American Physical Society", "publication": "Physical Review", "publication_date": "1965-12-06", "series_number": "5B", "volume": "140", "issue": "5B", "pages": "B1445-B1451" }, { "id": "authors:egn27-qcn32", "collection": "authors", "collection_id": "egn27-qcn32", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:BAHpr65b", "type": "article", "title": "Neutron Stars. II. Neutrino-Cooling and Observability", "author": [ { "family_name": "Bahcall", "given_name": "John N.", "clpid": "Bahcall-J-N" }, { "family_name": "Wolf", "given_name": "Richard A.", "orcid": "0000-0001-5291-4275", "clpid": "Wolf-Richard-A" } ], "abstract": "Calculations of the rates of the cooling reactions n+n\u2192n+p+e-+\u03bde and n+\u03c0-\u2192n+e-+\u03bde are presented; the rates of the closely related muon-producing reactions and the four inverse processes are also given. Several different arguments are used to obtain estimates of the relavant matrix elements. The nucleons are assumed to form a normal Fermi fluid with a continuous excitation spectrum. The calculated cooling rates indicate that a neutron star containing quasifree pions would cool within a few days to a temperature so low that the star would be unobservable. The surface of a star that does not contain quasifree pions would cool to 107 \u00b0K in a few months and would reach 4\u00d710^6 \u00b0K in about 100 years. The calculated cooling rates strongly indicate that the discrete x-ray sources located in the direction of the galactic center are not neutron stars.", "doi": "10.1103/PhysRev.140.B1452", "issn": "0031-899X", "publisher": "American Physical Society", "publication": "Physical Review", "publication_date": "1965-12-06", "series_number": "5B", "volume": "140", "issue": "5B", "pages": "B1452-B1466" }, { "id": "authors:yby8a-fqc72", "collection": "authors", "collection_id": "yby8a-fqc72", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120815-111016825", "type": "article", "title": "Neutron Stars", "author": [ { "family_name": "Bahcall", "given_name": "John N.", "clpid": "Bahcall-J-N" }, { "family_name": "Wolf", "given_name": "Richard A.", "orcid": "0000-0001-5291-4275", "clpid": "Wolf-Richard-A" } ], "abstract": "Several authors have suggested that the recently discovered extraterrestrial sources of x rays may be hot neutron stars. The plausibility of this suggestion, and in fact the likelihood\nthat astronomers will ever be able to observe neutron stars by their x-ray emission, depend critically upon the cooling times of the hot stars.", "doi": "10.1103/PhysRevLett.14.343", "issn": "0031-9007", "publisher": "American Physical Society", "publication": "Physical Review Letters", "publication_date": "1965-03-08", "series_number": "10", "volume": "14", "issue": "10", "pages": "343-346" }, { "id": "authors:a3d04-50d61", "collection": "authors", "collection_id": "a3d04-50d61", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151211-133226004", "type": "article", "title": "Observational Neutrino Astronomy", "author": [ { "family_name": "Bahcall", "given_name": "John N.", "clpid": "Bahcall-J-N" } ], "abstract": "This branch of astronomy will provide information that cannot be obtained by conventional observations.", "doi": "10.1126/science.147.3654.115", "issn": "0036-8075", "publisher": "American Association for the Advancement of Science", "publication": "Science", "publication_date": "1965-01-08", "series_number": "3654", "volume": "147", "issue": "3654", "pages": "115-120" }, { "id": "authors:3g6dr-fsj65", "collection": "authors", "collection_id": "3g6dr-fsj65", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120815-110844801", "type": "article", "title": "Neutrino Opacity. II. Neutrino-Nucleon Interactions", "author": [ { "family_name": "Bahcall", "given_name": "John N.", "clpid": "Bahcall-J-N" }, { "family_name": "Frautschi", "given_name": "Steven C.", "clpid": "Frautschi-S-C" } ], "abstract": "The contribution of neutrino-nucleon interactions to the neutrino opacity of matter is studied, special attention being paid to possible astrophysical applications such as supernova explosions. The results of recent accelerator experiments with high-energy neutrinos are used to show that nonresonant neutrino-nucleon scattering does not make a significant contribution to the neutrino opacity for astrophysically important conditions. The results of deep-mine cosmic-ray studies are then used to show that, (a) there are no resonances in the \u03bd_\u03bc-nucleon and \u03bd\u0305 _\u03bc-nucleon systems with masses less than 60 BeV (laboratory neutrino energies <2\u00d710^(+3) BeV), and (b) there are no resonances in the \u03bd_(e)-neucleon and \u03bd\u0305_(e)-nucleon systems with masses less than 7 BeV (laboratory neutrino energies <30 BeV). Neutrino absorption by bound nucleons is also discussed and a sum rule is proved for neutrino capture that is sufficiently accurate for most astrophysical applications. The effect of the exclusion principle on the capture cross sections is described and some applications to specific nuclei are presented. The accelerator experiments with high-energy neutrinos are then used to show that neutrino radioactivity, i.e., nuclear de-excitation by emission of a neutrino-antineutrino pair, is a substantially less important mechanism for stellar energy loss than was suggested by some previous estimates.", "doi": "10.1103/PhysRev.136.B1547", "issn": "0031-899X", "publisher": "American Physical Society", "publication": "Physical Review", "publication_date": "1964-12-07", "series_number": "5B", "volume": "136", "issue": "5B", "pages": "B1457-B1552" }, { "id": "authors:d9zpa-j6645", "collection": "authors", "collection_id": "d9zpa-j6645", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120817-114251049", "type": "article", "title": "Neutrino Opacity I. Neutrino-Lepton Scattering", "author": [ { "family_name": "Bahcall", "given_name": "John N.", "clpid": "Bahcall-J-N" } ], "abstract": "The contribution of neutrino-lepton scattering to the total neutrino opacity of matter is investigated; it is found that, contrary to previous beliefs, neutrino scattering dominates the neutrino opacity for many astrophysically important conditions. The rates for neutrino-electron scattering and antineutrino-electron scattering are given for a variety of conditions, including both degenerate and nondegenerate gases; the rates for some related reactions are also presented. Formulas are given for the mean scattering angle and the mean energy loss in neutrino and antineutrino scattering. Applications are made to the following problems: (a) the detection of solar neutrinos; (b) the escape of neutrinos from stars; (c) neutrino scattering in cosmology; and (d) energy deposition in supernova explosions.", "doi": "10.1103/PhysRev.136.B1164", "issn": "0031-899X", "publisher": "American Physical Society", "publication": "Physical Review", "publication_date": "1964-11-23", "series_number": "4B", "volume": "136", "issue": "4B", "pages": "B1164-B1171" }, { "id": "authors:ybx8y-wyc17", "collection": "authors", "collection_id": "ybx8y-wyc17", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141121-163839811", "type": "article", "title": "Nuclear matrix elements for the mirror decays of B^(12) and N^(12)", "author": [ { "family_name": "Eichler", "given_name": "J.", "clpid": "Eichler-J" }, { "family_name": "Tombrello", "given_name": "T. A.", "clpid": "Tombrello-T-A" }, { "family_name": "Bahcall", "given_name": "J. N.", "clpid": "Bahcall-J-N" } ], "abstract": "Recent precision experiments [1] have shown that the ft-value for the beta decay of N^(12) is significantly larger (11 \u00b1 1%) than the ft-value for the mirror beta decay of B^(12). Since this difference in ft-value has been used [2] in determining the coupling constants for induced pseudoscalar and induced tensor interactions in beta decay, assuming equality of the mirror matrix elements, it is important to investigate other effects that could cause the matrix elements themselves to be unequal. In this paper, we show that Coulomb effects alone, as manifested in single-particle binding energies, are large enough to account for the experimental difference in ft-values **.", "doi": "10.1016/0031-9163(64)90701-2", "issn": "0031-9163", "publisher": "Elsevier", "publication": "Physics Letters", "publication_date": "1964-11-15", "series_number": "2", "volume": "13", "issue": "2", "pages": "146-148" }, { "id": "authors:4mhdc-9pt65", "collection": "authors", "collection_id": "4mhdc-9pt65", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150908-150519805", "type": "article", "title": "Importance of a study of the decay of Ca^(37) to the problem of detecting solar neutrinos", "author": [ { "family_name": "Bahcall", "given_name": "J. N.", "clpid": "Bahcall-J-N" }, { "family_name": "Barnes", "given_name": "C. A.", "clpid": "Barnes-C-A" } ], "abstract": "Recent theoretical and experimental work has shown that a direct test of the theory of stellar energy generation in main sequence stars is possible by detecting solar neutrinos with the reaction Cl^(37) + ^v_(solar) \u2192 A^(37) e^-. In order to relate the counting rate in the proposed experiment to the flux of solar neutrinos (and thus ultimately to parameters describing the interior of the sun), one must know the matrix elements for neutrino\ncapture to all the relevant states in A^(37).", "doi": "10.1016/0031-9163(64)91171-0", "issn": "0031-9163", "publisher": "Elsevier", "publication": "Physics Letters", "publication_date": "1964-09-01", "series_number": "1", "volume": "12", "issue": "1", "pages": "48-49" }, { "id": "authors:byv6h-wqe19", "collection": "authors", "collection_id": "byv6h-wqe19", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:BAHpr64a", "type": "article", "title": "Neutrino astronomy and intermediate bosons", "author": [ { "family_name": "Bahcall", "given_name": "John N.", "clpid": "Bahcall-J-N" }, { "family_name": "Frautschi", "given_name": "Steven C.", "clpid": "Frautschi-S-C" } ], "abstract": "Neutrino fluxes from strong radio sources are estimated, assuming the neutrino-production mechanism: p+p\u2192nucleons+mesons\u2192nucleons+electrons, gamma rays, and neutrinos. The neutrino fluxes calculated on the basis of this mechanism are too small to be easily detected unless there are resonances in neutrino processes associated with the production of intermediate bosons. It is shown that a resonance in the antineutrino-electron system, associated with the usually hypothesized W- resonance, could be used to test, with standard experimental techniques, whether strong radio sources emit high-energy neutrinos in the quantities estimated in this paper. Two kinds of observational tests are described and counting rates are estimated. Observational tests of the kind we propose would provide important information about: (1) the mechanism for production of high-energy electrons in strong radio sources, and (2) the magnetic fields in such sources. Some comments concerning other logically possible neutrino resonances are also included.", "doi": "10.1103/PhysRev.135.B788", "issn": "0031-899X", "publisher": "Physical Review", "publication": "Physical Review", "publication_date": "1964-08-10", "series_number": "3B", "volume": "135", "issue": "3B", "pages": "B788-B791" }, { "id": "authors:5f564-fbh35", "collection": "authors", "collection_id": "5f564-fbh35", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120817-095113210", "type": "article", "title": "Solar Neutrino Cross Sections and Nuclear Beta Decay", "author": [ { "family_name": "Bahcall", "given_name": "John N.", "clpid": "Bahcall-J-N" } ], "abstract": "The neutrino-producing reactions that are believed to occur in the interior of the sun are reviewed and\nthe predicted neutrino fluxes from these reactions are presented. The relevant absorption cross sections for\nneutrino-induced transitions from the ground state of Cl^(37) to various states in Ar^(37) are then calculated. The nuclear model adopted in these calculations is also used to predict the decay rates and branching ratios\nfor a number of nuclei with 1d^(n)_(3/2) configurations; comparisons with experiment are made wherever possible\nand additional tests are suggested. A method for extracting Gamow-Teller matrix elements from mixed transitions between members of the same isotopic multiplet is then illustrated. The theory of bound-state neutrino capture is also outlined and applied to the proposed solar neutrino experiment. In an Appendix, some neutrino cross sections that are useful in interpreting the reactor experiment of Davis are presented.", "doi": "10.1103/PhysRev.135.B137", "issn": "0031-899X", "publisher": "American Physical Society", "publication": "Physical Review", "publication_date": "1964-07-13", "series_number": "1B", "volume": "135", "issue": "1B", "pages": "B137-B146" }, { "id": "authors:rftaf-zfs56", "collection": "authors", "collection_id": "rftaf-zfs56", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120815-115103844", "type": "article", "title": "Solar Neutrinos. I. Theoretical", "author": [ { "family_name": "Bahcall", "given_name": "John N.", "clpid": "Bahcall-J-N" } ], "abstract": "The principal energy source for main-sequence\nstars like the sun is believed to be the fusion, in\nthe deep interior of the star, of four protons to\nform an alpha particle. The fusion reactions\nare thought to be initiated by the sequence ^1H(p,\ne^(+)v)^2H(p,\u03b3)^(3)He and terminated by the following\nsequences: (i) ^(3)He(^(3)He, 2p)^(4)He; (ii) ^(3)He(\u03b1,\u03b3)^(7)Be(e^(-)v)^(7)Li(p,\u03b1)^(4)He; and (iii) ^(3)He(\u03b1,\u03b3)^(7)Be(p,\u03b3)^(8)B(e^(+)v)^(8)Be*(\u03b1)^(4)He. No direct evidence for the existence of nuclear reactions in the interiors of stars has yet been obtained because the mean free path for photons emitted in the center of a star is typically less than 10^(-10) of the radius of\nthe star. Only neutrinos, with their extremely\nsmall interaction cross sections, can enable us\nto see into the interior of a star and thus verify\ndirectly the hypothesis of nuclear energy generation\nin stars.", "doi": "10.1103/PhysRevLett.12.300", "issn": "0031-9007", "publisher": "American Physical Society", "publication": "Physical Review Letters", "publication_date": "1964-03-16", "series_number": "11", "volume": "12", "issue": "11", "pages": "300-302" }, { "id": "authors:wpvzt-5jb94", "collection": "authors", "collection_id": "wpvzt-5jb94", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:BAHpr63c", "type": "article", "title": "Exchange and overlap effects in electron capture and in related phenomena", "author": [ { "family_name": "Bahcall", "given_name": "John N.", "clpid": "Bahcall-J-N" } ], "abstract": "Theoretical expressions are presented for L/K electron capture ratios and electron capture-positron emission ratios that include the effects of electron exchange and imperfect atomic overlap. The role of electron exchange and imperfect atomic overlap in the determination of fluorescence yields is also discussed. In order to facilitate experimental comparisons, numerical values are presented for the exchange and overlap corrections to L/K ratios and electrons capture-positron emission ratios; these correctiosn were calculated with the analytic Hartree-Fock wave functions of Watson and Freeman. The corrected L/K ratios are in good agreement with the precisely measured L/K ratios, showing that overlap and exchange corrections explain the systematic disagreement between the predictions of the usual electron capture theory and experiment.", "doi": "10.1103/PhysRev.132.362", "issn": "0031-899X", "publisher": "Physical Review", "publication": "Physical Review", "publication_date": "1963-10-01", "series_number": "1", "volume": "132", "issue": "1", "pages": "362-367" }, { "id": "authors:9dras-k9q97", "collection": "authors", "collection_id": "9dras-k9q97", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:BAHpr63b", "type": "article", "title": "Effect of exchange on M/L electron capture ratios", "author": [ { "family_name": "Bahcall", "given_name": "John N.", "clpid": "Bahcall-J-N" } ], "abstract": "Theoretical expressions that include the effect of electron exchange are given for M/L electron-capture ratios; the results are presented in a form that makes clear the physical origin of the exchange corrections. Accurate values for M/L ratios both with and without exchange corrections are tabulated for Z between 13 and 37; these numerical results were calculated using the analytic Hartree-Fock wave functions of Watson and Freeman. The exchange correction for Z greater than or equal to 38 has been estimated by a least squares extrapolation of the correction for lower Z values. The effect of electron exchange on electron capture to positron-emission ratios is also discussed. The exchange-corrected theoretical M/L ratio for 32Ge71 is 0.173, in disagreement with the recent measurement of Manduchi and Zannoni. It is suggested that some additional precision measurements of M/L ratios be performed in order to clarify this discrepancy between theory and experiment.", "doi": "10.1103/PhysRev.131.1756", "issn": "0031-899X", "publisher": "Physical Review", "publication": "Physical Review", "publication_date": "1963-08-15", "series_number": "4", "volume": "131", "issue": "4", "pages": "1756-1759" }, { "id": "authors:19xjd-bwy82", "collection": "authors", "collection_id": "19xjd-bwy82", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:BAHpr63a", "type": "article", "title": "Overlap and exchange effects in beta decay", "author": [ { "family_name": "Bahcall", "given_name": "John N.", "clpid": "Bahcall-J-N" } ], "abstract": "The change in nuclear charge by one unit in beta decay causes initial and final atomic states to overlap imperfectly. The effect of this imperfect overlap on the shape of allowed electron and positron emission spectra is calculated. The calculated change in the spectrum shape can be simulated by including the average excitation energy of the final atom in the energy balance. The inhibition, due to imperfect atomic overlap, of electron-capture rates, as well as total electron and positron-emission rates, is also determined. In all known cases, imperfect atomic overlap increases beta-decay lifetimes by at most a few percent and usually by an amount less than a few tenths of one percent. Antisymmetrization between decay and bound atomic electrons, in conjunction with the change in nuclear charge, gives rise to exchange effects in electron emission and electron capture. Due to exchange terms, the usual allowed electron spectrum is multiplied by a quantity that is of the order of 1-2Z-1 for energies less than the binding energy of a K electron in the initial atom. This exchange correction is negligible for higher energies of the emitted continuum electron. A simple approximate formula is derived that predicts the effect of exchange on L to K capture ratios; this formula predicts a 22% increase over the usual theoretical value for the L to K ratio of Ar37. The Ar37 prediction is in excellent agreement with recent experiments and with a more complicated calculation by Odiot and Daudel. Exchange effects change total electron emission and electron capture rates by at most a few percent.", "doi": "10.1103/PhysRev.129.2683", "issn": "0031-899X", "publisher": "Physical Review", "publication": "Physical Review", "publication_date": "1963-03-15", "series_number": "6", "volume": "129", "issue": "6", "pages": "2683-2694" }, { "id": "authors:a6yr5-wgs10", "collection": "authors", "collection_id": "a6yr5-wgs10", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:BAHprl62", "type": "article", "title": "Effect of Exchange on L to K Capture Ratios", "author": [ { "family_name": "Bahcall", "given_name": "John N.", "clpid": "Bahcall-J-N" } ], "abstract": "Two years ago, Robinson and Fink (1) called attention to a systematic discrepancy between observed and predicted L to K electron capture ratios. Many experiments have since been performed to investigate this discrepancy. The observed L to K ratio has been found (2-5) to exceed 5 to 25 percent the predicted L to K ratio for all nine of the precisely measured allowed electron captures with Z between 18 and 36. The calculations reported in this note remove the systematic disagreement between theory and experiment by including atomic states in the description of the radioactive system.", "doi": "10.1103/PhysRevLett.9.500", "issn": "0031-9007", "publisher": "American Physical Society", "publication": "Physical Review Letters", "publication_date": "1962-12-15", "series_number": "12", "volume": "9", "issue": "12", "pages": "500-502" } ]