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Neutron Stars. II. Neutrino-Cooling and Observability

Bahcall, John N. and Wolf, Richard A. (1965) Neutron Stars. II. Neutrino-Cooling and Observability. Physical Review, 140 (5B). B1452-B1466. ISSN 0031-899X. doi:10.1103/PhysRev.140.B1452.

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Calculations of the rates of the cooling reactions n+n→n+p+e-+νe and n+π-→n+e-+νe 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 °K in a few months and would reach 4×10^6 °K 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.

Item Type:Article
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Wolf, Richard A.0000-0001-5291-4275
Additional Information:© 1965 The American Physical Society. Received 19 July 1965. We are grateful to Dr. A.G.W. Cameron and Dr. S. Tsuruta, and to Dr. R. Giacconi and Dr. H. Gursky for informing us of their work prior to publication. Supported in part by the Office of Naval Research Nonr-220(47) and the National Aeronautics and Space Administration NGR-05-002-028. [R.A.W. was a] National Science Foundation Predoctoral Fellow in Physics
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Office of Naval Research (ONR)Nonr-220(47)
NSF Graduate Research FellowshipUNSPECIFIED
Issue or Number:5B
Record Number:CaltechAUTHORS:BAHpr65b
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ID Code:11906
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Deposited On:09 Oct 2008 18:30
Last Modified:08 Nov 2021 22:23

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