Three Types of Cooling Superfluid Neutron Stars: Theory and Observations

Abstract

Cooling of neutron stars (NSs) with the cores composed of neutrons, protons, and electrons is simulated assuming ${}^1$S${}_0$ pairing of neutrons in the NS crust, and also ${}^1$S${}_0$ pairing of protons and weak ${}^3$P${}_2$ pairing of neutrons in the NS core, and using realistic density profiles of the superfluid critical temperatures $T_{\mathrm{c}}(\rho )$. The theoretical cooling models of isolated middle-aged NSs can be divided into three main types. (I) {\it Low-mass}, {\it slowly cooling} NSs where the direct Urca process of neutrino emission is either forbidden or almost fully suppressed by the proton superfluidity. (II) {\it Medium-mass} NSs which show {\it moderate} cooling via the direct Urca process suppressed by the proton superfluidity. (III) {\it Massive} NSs which show {\it 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 $T_{\mathrm{c}}(\rho )$ 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, $T_{\mathrm{cp}}(\rho )$, and the equation of state in the NS core. No rapidly cooling NS has been observed so far.

12 pages, 10 figures, Astron. Astrophys., submitted

References in corpus (2)

• The Chandra LETGS high resolution X-ray spectrum of the isolated neutron star RX J1856.5-3754
• ${}^1$S${}_0$ Neutron Pairing vs Observations of Cooling Neutron Stars

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