All Figures

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{f1h3958.ps}\end{figure}$ Figure 1: Observational limits on surface temperatures of eight NSs versus toy-model cooling curves of low-mass NSs (solid lines) with two slow neutrino emission levels and high-mass NSs (long dashes) with three fast neutrino emission levels. Dashed-and-dot line: slow cooling of a nonsuperfluid 1.4 $M_\odot$ NS calculated with the exact cooling code; dotted line: the same but assuming triplet-state neutron pairing in the core, Takatsuka (1972) model; short-dashes: the same but with strong proton pairing and nonsuperfluid neutrons.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.15cm,clip]{f2h3958.ps}\end{figure}$ Figure 2: Transition from slow to fast cooling with increasing NS mass over the threshold value $M_{\rm s}$ for the same values of $Q_{\rm s}$ and $Q_{\rm f}$ as in Fig. 1 and two transition density intervals, $\Delta \rho /\rho _{\rm s}=0.01$ or 0.1, at a fixed NS age t=25 000 yrs. Shaded strip: observational limits for the Vela pulsar.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.15cm,clip]{f2h3958.ps}\end{figure}$	Figure 2: Transition from slow to fast cooling with increasing NS mass over the threshold value $M_{\rm s}$ for the same values of $Q_{\rm s}$ and $Q_{\rm f}$ as in Fig. 1 and two transition density intervals, $\Delta \rho /\rho _{\rm s}=0.01$ or 0.1, at a fixed NS age t=25 000 yrs. Shaded strip: observational limits for the Vela pulsar.
Open with DEXTER