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Neutron star cooling: Theoretical aspects and observational constraints

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arxiv astro-ph/0306143 v1 pith:RE6XWI33 submitted 2003-06-06 astro-ph

D. G. Yakovlev (1) , O. Y. Gnedin (2) , A. D. Kaminker (1) , K. P. Levenfish (1) , A. Y. Potekhin (1) ((1) Ioffe Phys.-Tech. Institute , St. Petersburg; (2) STScI) This is my paper · ORCID
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keywords coolingneutronmatterstarsdiscussedinteriorsisolatedtheory
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The cooling theory of isolated neutron stars is reviewed. The main cooling regulators are discussed, first of all, operation of direct Urca process (or similar processes in exotic phases of dense matter) and superfluidity in stellar interiors. The prospects to constrain gross parameters of supranuclear matter in neutron-star interiors by confronting cooling theory with observations of isolated neutron stars are outlined. A related problem of thermal states of transiently accreting neutron stars with deep crustal heating of accreted matter is discussed in application to soft X-ray transients.

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Cited by 2 Pith papers

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    Magnetic fields up to 5e17 G increase charged-current neutrino and antineutrino opacities in neutron star merger matter by up to two orders of magnitude at low temperature, shrinking neutrino mean free paths.

  2. Probing freeze-in dark matter using Bose-Einstein condensate in neutron star

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    Bose-Einstein condensate formation in neutron stars enhances dark matter annihilation by 10^15-10^20, allowing freeze-in models to produce observable heating and probe neutrino-fog scattering cross-sections.

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