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$\begin{figure} \par\epsfxsize=15cm \epsffile{3628fig1.eps} \end{figure}$ Figure 1: The redshifted effective surface temperature versus the internal temperature for a canonical neutron star ( $M=1.4~M_\odot$ , R=10 km) with the magnetic field B=10⁸, 10¹², and 10¹⁴ G ( left, middle, and right panels) and for the case of dipole (dot-dash lines) and small-scale (solid lines) fields. The upper and lower curves represent the accreted and iron heat-blanketing envelope, respectively.
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In the text

$\begin{figure} \par\epsfxsize=70mm \epsffile{3628fig2.eps} % \end{figure}$ Figure 2: The dependence of the mean effective temperature on B for the dipole (dot-dash lines) and small-scale (solid lines) fields. The curves are shown for the accreted and iron envelopes and the internal temperature $T_{\rm b}=10^7$ K and 10⁸ K (marked near the curves).
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In the text

$\begin{figure} \par\epsfxsize=70mm \epsffile{3628fig2.eps} % \end{figure}$	Figure 2: The dependence of the mean effective temperature on B for the dipole (dot-dash lines) and small-scale (solid lines) fields. The curves are shown for the accreted and iron envelopes and the internal temperature $T_{\rm b}=10^7$ K and 10⁸ K (marked near the curves).
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