![\begin{figure}
\par\includegraphics[width=16cm,clip]{1006f1.ps}
\end{figure}](/articles/aa/full/2004/33/aa1006/img19.gif) |
Figure 1: Left: density dependence of the critical temperature of model p1 for proton superfluidity and model nt1 for neutron superfluidity in a neutron-star core; the vertical dot-and-dash line indicates the central density of a maximum-mass neutron star. Right: observations (Table 1) compared with theoretical cooling curves of eight neutron stars (1-8) with different masses. All solid curves refer to neutron stars with model superfluidities from the left panel. The dotted curve 7 is for a non-superfluid star. The insert table gives masses and central densities of stars 1-8. |
| Open with DEXTER | |
In the text
![\begin{figure}
\par\includegraphics[width=8cm,clip]{1006f2.ps}
\end{figure}](/articles/aa/full/2004/33/aa1006/img84.gif) |
Figure 2:
A sketch of neutrino luminosities produced
by the modified Urca process (
 )
and the Cooper pairing process (
 )
as well as of the photon luminosity 
of a neutron star versus internal temperature T for three models of neutron superfluidity in the stellar
core with
 ,
and
109 K. |
| Open with DEXTER | |
In the text
![\begin{figure}
\par\includegraphics[width=16cm,clip]{1006f3.ps}
\end{figure}](/articles/aa/full/2004/33/aa1006/img100.gif) |
Figure 3:
Left: One model p1 for proton superfluidity
and five models nt1-nt5 for neutron superfluidity
in a neutron-star core. Right: Cooling curves
of low-mass (1.111  )
and
high-mass (1.994 )
stars with model p1 proton superfluidity
and one of the models of neutron superfluidity from the left
panel, compared with the observations. Cooling of the low-mass
star is insensitive to selected models of neutron superfluidity
(except for model nt2 at t > 300 kyr).
The insert shows the comparison of cooling curves of the high-mass star
with observations of the Vela pulsar in more detail. |
| Open with DEXTER | |
In the text