All Figures

$\begin{figure} \par\includegraphics[width=6cm,bb=0 166 355 509,clip]{1283fig1.eps} \end{figure}$ Figure 1: Geometry of the post-shock region model.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1283fig2.ps} \end{figure}$ Figure 2: Temperature and density profiles for one of the PSR models. The dashed lines show a simple analytic solution of the structure of the post shock region (Frank et al. 2002).
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{1283fg3a.ps}\hspace*{3mm} \i... ...fg3e.ps}\hspace*{3mm} \includegraphics[width=7cm,clip]{1283fg3f.ps} \end{figure}$ Figure 3: Spectra of intermediate polars obtained with the RXTE observatory. Crosses denote PCA data, open circles - HEXTE data. The solid lines show the best fit model with parameters presented in Table 1.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{1283fg4a.ps}\hspace*{3mm} \i... ...fg4e.ps}\hspace*{3mm} \includegraphics[width=7cm,clip]{1283fg4f.ps} \end{figure}$ Figure 4: The same as Fig. 3.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{1283fg5a.ps}\hspace*{3mm} \includegraphics[width=7cm,clip]{1283fg5b.ps} \end{figure}$ Figure 5: The same as Fig. 3.
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In the text

$\begin{figure} \includegraphics[width=8.1cm,clip]{1283fig6.ps} \end{figure}$ Figure 6: Comparison of the masses of the white dwarfs as estimated from RXTE broadband spectra (this work) with estimates obtained by other methods. (1) - Beuermann et al. (2003); (2) - Crampton et al. (1986); (3) - Reinsch (1994); (4) - Haswell et al. (1997); (5) - Mateo et al. (1991); (6) - Friend et al. (1990); (7) - Hellier (1993); (8) - Penning (1985).
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In the text

$\begin{figure} \par\includegraphics[width=6cm,bb=0 166 355 509,clip]{1283fig1.eps} \end{figure}$	Figure 1: Geometry of the post-shock region model.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{1283fig2.ps} \end{figure}$	Figure 2: Temperature and density profiles for one of the PSR models. The dashed lines show a simple analytic solution of the structure of the post shock region (Frank et al. 2002).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7cm,clip]{1283fg3a.ps}\hspace{3mm} \i... ...fg3e.ps}\hspace{3mm} \includegraphics[width=7cm,clip]{1283fg3f.ps} \end{figure}$	Figure 3: Spectra of intermediate polars obtained with the RXTE observatory. Crosses denote PCA data, open circles - HEXTE data. The solid lines show the best fit model with parameters presented in Table 1.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7cm,clip]{1283fg4a.ps}\hspace{3mm} \i... ...fg4e.ps}\hspace{3mm} \includegraphics[width=7cm,clip]{1283fg4f.ps} \end{figure}$	Figure 4: The same as Fig. 3.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{1283fg5a.ps}\hspace*{3mm} \includegraphics[width=7cm,clip]{1283fg5b.ps} \end{figure}$	Figure 5: The same as Fig. 3.
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$\begin{figure} \includegraphics[width=8.1cm,clip]{1283fig6.ps} \end{figure}$	Figure 6: Comparison of the masses of the white dwarfs as estimated from RXTE broadband spectra (this work) with estimates obtained by other methods. (1) - Beuermann et al. (2003); (2) - Crampton et al. (1986); (3) - Reinsch (1994); (4) - Haswell et al. (1997); (5) - Mateo et al. (1991); (6) - Friend et al. (1990); (7) - Hellier (1993); (8) - Penning (1985).
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