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Cooling of neutron starsIt is at present impossible to predict the interior constitution of neutron stars based on theory and results from laboratory studies. It has been proposed that it is possible to obtain information on neutron star interiors by studying thermal radiation from their surfaces, because neutrino emission rates, and hence the temperature of the central part of a neutron star, depend on the properties of dense matter. The theory predicts that neutron stars cool relatively slowly if their cores are made up of nucleons, and cool faster if the matter is in an exotic state, such as a pion condensate, a kaon condensate, or quark matter. This view has recently been questioned by the discovery of a number of other processes that could lead to copious neutrino emission and rapid cooling.
Document ID
19930066501
Document Type
Reprint (Version printed in journal)
Authors
Pethick, C. J.
(NORDITA, Copenhagen, Denmark; Illinois Univ. Urbana, United States)
Date Acquired
August 16, 2013
Publication Date
October 1, 1992
Publication Information
Publication: Reviews of Modern Physics
Volume: 64
Issue: 4
ISSN: 0034-6861
Subject Category
Astrophysics
Accession Number
93A50498
Funding Number(s)
CONTRACT_GRANT: NAGW-1583
CONTRACT_GRANT: NSF PHY-91-00283
Distribution Limits
Public
Copyright
Other

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