| Issue |
A&A
Volume 373, Number 2, July II 2001
|
|
|---|---|---|
| Page(s) | L17 - L20 | |
| Section | Letters | |
| DOI | https://doi.org/10.1051/0004-6361:20010713 | |
| Published online | 15 July 2001 | |
Nucleon superfluidity vs. observations of cooling neutron stars
1
Ioffe Physical Technical Institute, Politekhnicheskaya 26, 194021 St. Petersburg, Russia
2
N. Copernicus Astronomical Center, Bartycka 18, 00-716 Warsaw, Poland e-mail: haensel@camk.edu.pl; yak@astro.ioffe.rssi.ru
Corresponding author: A. D. Kaminker, kam@astro.ioffe.rssi.ru
Received:
30
April
2001
Accepted:
18
May
2001
Cooling simulations of neutron stars (NSs) are performed
assuming that stellar cores consist of neutrons, protons
and electrons and using realistic density profiles
of superfluid critical temperatures
and 
of neutrons and protons.
Taking a suitable profile of
with maximum ~
K one can
obtain smooth transition from slow to rapid cooling
with increasing stellar mass. Adopting
the same profile one can explain the majority of observations of thermal
emission from isolated middle-aged
NSs by cooling
of NSs with different masses either
with no neutron superfluidity in the cores
or with a weak superfluidity, 
K.
The required masses range from ~
for
(young and hot) RX J0822-43 and
(old and warm) PSR 1055-52
and RX J1856-3754
to ≈
for the (rather cold) Geminga and Vela pulsars.
Observations constrain the
and profiles with respect to
the threshold density of direct Urca process
and maximum central density of NSs.
Key words: stars: neutron / dense matter
© ESO, 2001
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