All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{f1h3959.ps} \end{figure}$ Figure 1: Simultaneous calculation of cooling and heating curves for low-mass (thick lines) and high-mass (thin lines) NS models (see the text). Displayed are: the neutrino, photon and total luminosities, $L_\nu ^\infty$ , $L_\gamma ^\infty$ and $L_{\rm tot}^\infty$ (left vertical scale), of a cooling NS versus its age, and the accretion rate $\dot{M}$ (right vertical scale) of an accreting NS star with $L_{\rm dh}^\infty =L_{\rm tot}^\infty$ . Dotted horizontal line: $L_{\rm dh}^\infty$ for $\dot{M}=10^{-10}$ $M_\odot$ yr^-1. Filled circles and dotted vertical arrows refer to those low-mass and high-mass cooling NSs which are equivalent to accreting NSs with the indicated $\dot{M}$ ; open circles: $L_\gamma ^\infty$ for these cooling NSs.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{f2h3959.ps} \end{figure}$ Figure 2: Heating curves of accreting NSs compared with observations of several SXRTs in quiescence. Thick solid line: deep crustal heating power, $L_{\rm dh}$ . Long dashes and thin solid lines: two models of heating curves of low-mass NSs ( $Q_{\rm s}=3 \times 10^{19}$ and 10²¹). Dotted, short-dashed, and dot-and-dashed lines: three models of high-mass NSs ( $Q_{\rm f}=10^{23}$ , 10²⁵, and 10²⁷).
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In the text