Neutron star cooling

A. D. Kaminker (1); A. Y. Potekhin (1) ((1) Ioffe Phys.-Tech. Institute; D. G. Yakovlev (1); K. P. Levenfish (1); M. E. Gusakov (1); O. Y. Gnedin (2); St. Petersburg; (2) Ohio State University)

arxiv: astro-ph/0409751 · v1 · submitted 2004-09-30 · 🌌 astro-ph · nucl-th

Neutron star cooling

D. G. Yakovlev (1) , O. Y. Gnedin (2) , M. E. Gusakov (1) , A. D. Kaminker (1) , K. P. Levenfish (1) , A. Y. Potekhin (1) ((1) Ioffe Phys.-Tech. Institute , St. Petersburg; (2) Ohio State University) This is my paper

classification 🌌 astro-ph nucl-th

keywords neutroncoolingmatterstarstarstheoreticalanalyzedbaryon

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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.

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Neutron star cooling

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