Neutron star cooling

descriptionPublicationkeyboard_double_arrow_right Article , Preprint 01 Apr 2005Embargo end date: 01 Sep 2004 English Publisher:Elsevier BVJournal:Nuclear Physics A, volume 752, pages 590-599 (issn: 0375-9474,

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Authors: Yakovlev, D. G.; Gnedin, O. Y.; Gusakov, M. E.; Kaminker, A. D.; Levenfish, K. P.; Potekhin, A. Y.;

doi: 10.1016/j.nuclphysa.2005.02.061 , 10.48550/arxiv.astro-ph/0409751

arXiv: astro-ph/0409751

Neutron star cooling

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Abstract

The impact of nuclear physics theories on cooling of isolated neutron stars is analyzed. Physical properties of neutron star matter important for cooling are reviewed such as composition, the equation of state, superfluidity of various baryon species, neutrino emission mechanisms. Theoretical results are compared with observations of thermal radiation from neutron stars. Current constraints on theoretical models of dense matter, derived from such a comparison, are formulated.

10 pages, 8 figures, to appear in Proceedings of the International Nuclear Physics Conference (INPS2004) (Goeteborg, Sweden, June 27 - July 2, 2004)

Related Organizations

Ioffe Physico-Technical Institute
Russian Federation
The Ohio State University
United States
Physico-Technical Institute
Russian Federation
Ural Branch of the Russian Academy of Sciences
Russian Federation

Keywords

Nuclear Theory (nucl-th), Nuclear Theory, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics

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