Astronomy & Astrophysics

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Issue		A&A Volume 383, Number 3, March I 2002
Page(s)		1076 - 1087
Section		Physical and chemical processes
DOI		10.1051/0004-6361:20011797

A&A 383, 1076-1087 (2002)
DOI: 10.1051/0004-6361:20011797

Three types of cooling superfluid neutron stars: Theory and observations

A. D. Kaminker¹, D. G. Yakovlev¹ and O. Y. Gnedin²

¹ Ioffe Physical Technical Institute, Politekhnicheskaya 26, 194021 St. Petersburg, Russia
² Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
e-mail: yak@astro.ioffe.rssi.ru; ognedin@stsci.edu

(Received 21 November 2001 / Accepted 17 December 2001 )

Abstract
Cooling of neutron stars (NSs) with the cores composed of neutrons, protons, and electrons is simulated assuming ¹S ₀ pairing of neutrons in the NS crust, and also ¹S ₀ pairing of protons and weak ³P ₂ pairing of neutrons in the NS core, and using realistic density profiles of the superfluid critical temperatures $T_{\rm c}(\rho)$ . The theoretical cooling models of isolated middle-aged NSs can be divided into three main types. (I) Low-mass, slowly cooling NSs where the direct Urca process of neutrino emission is either forbidden or almost fully suppressed by the proton superfluidity. (II) Medium-mass NSs which show moderate cooling via the direct Urca process suppressed by the proton superfluidity. (III) Massive NSs which show fast cooling via the direct Urca process weakly suppressed by superfluidity. Confronting the theory with observations we treat RX J0822-43, PSR 1055-52 and RX J1856-3754 as slowly cooling NSs. To explain these sufficiently warm sources we need a density profile $T_{\rm c}(\rho)$ in the crust with a rather high and flat maximum and sharp wings. We treat 1E 1207-52, RX J0002+62, PSR 0656+14, Vela, and Geminga as moderately cooling NSs. We can determine their masses for a given model of proton superfluidity, $T_{\rm cp}(\rho)$ , and the equation of state in the NS core. No rapidly cooling NS has been observed so far.

Key words: stars: neutron -- dense matter

Offprint request: A. D. Kaminker, kam@astro.ioffe.rssi.ru

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