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arXiv · astro-ph/0204226

Cooling of Superfluid Neutron Stars

D. G. Yakovlev·O. Y. Gnedin·A. D. Kaminker·A. Y. Potekhin
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Abstract

Cooling of neutron stars (NSs) with the cores composed of neutrons, protons, and electrons is analyzed. The main cooling regulators are discussed: opening of direct Urca process in a NS central kernel; superfluidity of nucleons in NS interiors; surface layers of light (accreted) elements; strong surface magnetic fields. An emphasis is paid on the cooling scenario with strong $^1$S$_0$ pairing of protons and weak $^3$P$_2$ pairing of neutrons in the NS core, as well as strong $^1$S$_0$ pairing of neutrons in the NS crust. The theory predicts three types of isolated cooling middle-aged NSs with distinctly different properties: low-mass, slowly cooling NSs; medium-mass, moderately cooling NSs; massive, rapidly cooling NSs. The theory is compared with observations of isolated NSs -- pulsars and radio quiet NSs in supernova remnants. The constraints on physical properties of NSs which can be inferred from such a comparison are outlined.

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BibTeXRIS

D. G. Yakovlev, O. Y. Gnedin, A. D. Kaminker, A. Y. Potekhin. 2002-04-13. Cooling of Superfluid Neutron Stars. https://arxiv.org/abs/astro-ph/0204226

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