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Thermal Properties of Neutron Stars

Published online by Cambridge University Press:  14 August 2015

S. Tsuruta
S. Tsuruta*
Affiliation:
NORDITA, Copenhagen, Denmark Department of Physics, Montana State University, Bozeman, Montana, U.S.A.

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The problem of neutron star thermodynamics has become a rather hot issue during the last one to two years, mainly because the enormous technological improvements brought by the Einstein Observatory (HEAO-B) and the exciting data which have become available to us through this satellite have given us a better hope of testing some of neutron star theories, which may eventually give us invaluable insight into various fields of physics. A somewhat extensive review of the pre-Einstein (Observatory) days was given in Tsuruta (1979a). Since then, many papers, both observational and theoretical, have come out. Most of the observational papers are reports from the Einstein Observatory. Stimulated by such progress on the observational side, various authors of recent theoretical papers attempted to reinvestigate and (or) improve the cooling and heating theories. Dave Helfand (1981) has already given a comprehensive summary of the most recent developments in heating theories. Therefore, in our present report, we shall restrict ourselves to the most recent developments in cooling theories and the comparison with the latest observations. The reader is referred to the earlier reviews (e.g. Tsuruta 1979a, b, 1980a) for the earlier work and the details.

Type
VII. Properties of Neutron Stars
Information
Symposium - International Astronomical Union , Volume 95: Pulsars , 1981 , pp. 331 - 337
Copyright
Copyright © Reidel 1981 

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