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A&A 389, L24-L27 (2002)
DOI: 10.1051/0004-6361:20020699
Letter
The cooling neutron star in 3C 58
D. G. Yakovlev1, A. D. Kaminker1, P. Haensel2 and O. Y. Gnedin31 Ioffe Physical Technical Institute, Politekhnicheskaya 26, 194021 St. Petersburg, Russia
e-mail: kam@astro.ioffe.rssi.ru
2 N. Copernicus Astronomical Center, Bartycka 18, 00-716 Warsaw, Poland
e-mail: haensel@camk.edu.pl
3 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
e-mail: ognedin@stsci.edu
(Received 15 April 2002 / Accepted 13 May 2002)
Abstract
The upper limit on 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 observations 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 that provided by
the well known observations of Vela and Geminga.
Key words: pulsars: individual: PSR J0205+6449 -- stars: neutron -- dense matter
Offprint request: D. G. Yakovlev, yak@astro.ioffe.rssi.ru
SIMBAD Objects
© ESO 2002
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