The Cooling Neutron Star in 3C 58

Details The Cooling Neutron Star in 3C 58 The Cooling Neutron Star in 3C 58

2002-04-15

arxiv.org/abs/astro-ph/0204233v2

Astron.Astrophys. 389 (2002) L24

Astronomy and Astrophysics

Astrophysics

3 pages, 2 figures, AA Letters (submitted)

Scientific paper

10.1051/0004-6361:20020699

The upper limit of the effective surface temperature of the neutron star (NS) PSR J0205+6449 in the supernova remnant 3C 58 obtained recently by Slane et al. (2002) is analyzed using a modern theory of NS cooling (Kaminker et al. 2002). The observational limit can be explained by cooling of a superfluid NS with the core composed of neutrons, protons and electrons, where direct Urca process is forbidden. However, combined with the data on the surface temperatures of other isolated NSs, it gives evidence (emphasized by Slane et al.) that direct Urca process is open in the inner cores of massive NSs. This evidence turns out to be less stringent than the evidence provided by the well known observations of Vela and Geminga.

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