Cooling of Superfluid Neutron Stars

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dc.creatorYakovlev, D. G.
dc.creatorGnedin, O. Y.
dc.creatorKaminker, A. D.
dc.creatorPotekhin, A. Y.
dc.date2002-04-13
dc.date.accessioned2026-07-07T02:03:24Z
dc.date.available2026-07-07T02:03:24Z
dc.descriptionCooling 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.
dc.description14 pages, 13 figures, he_symp; to be published in Proceedings of the 270. Heraeus Seminar on Neutron Stars, Pulsars and Supernova Remnants, Bad Honnef, Jan. 21-25, 2002
dc.identifierhttps://arxiv.org/abs/astro-ph/0204226
dc.identifierhttp://arxiv.org/abs/astro-ph/0204226
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/4373
dc.subjectAstrophysics
dc.titleCooling of Superfluid Neutron Stars
dc.typetext

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