All Figures

$\begin{figure} \par\includegraphics[width=6.4cm,clip]{5102fig1.eps} \end{figure}$ Figure 1: Spectra a) and temperature structures b) of a hot DA white dwarf model atmosphere with $T_{\rm eff}= 200~ 000$ K and $\log~g = 6.3$ with (solid line) and without (dashed line) Compton scattering taken into account.
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,height=10.5cm,clip]{5102fig2.eps} \end{figure}$ Figure 2: Spectra a) of the DA white dwarf HZ 43 model atmosphere with (solid line) and without (dashed line) Compton scattering using Method 1. Also shown are the spectra of the non-LTE model atmosphere (dotted line) and the spectra of non-LTE model atmosphere with Compton scattering (open circles). Run b) of Comptonisation parameter $Z_{\rm Compt}$ with wavelength (see Eq. (19)).
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{5102fig3.eps} \end{figure}$ Figure 3: Emergent X-ray spectra for a pure hydrogen model atmosphere appropriate for the parameters of HZ 43 computed for classical Thomson scattering (dashed) and Compton scattering (solid) using Method 2 (the method of Madej et al. 2004).
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{5102fig4.eps} \end{figure}$ Figure 4: The same as Fig. 2 but here for the DA white dwarf Sirius B LTE model atmosphere. The dotted line lies everywhere under the open circles (except for hydrogen lines).
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{5102fig5.eps} \end{figure}$ Figure 5: Spectra a) of the DA white dwarf $T_{\rm eff} = 100~ 000$ K model atmospheres with and without Compton scattering. Solid lines correspond to model with $\log~g=8.0$ , and dashed lines correspond to model with $\log~g = 6.0$ . Softer high energy tails correspond to models with Compton effect. Run b) of Comptonisation parameter $Z_{\rm Compt}$ with wavelength.
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In the text

$\begin{figure} \par\includegraphics[width=6.4cm,clip]{5102fig1.eps} \end{figure}$	Figure 1: Spectra a) and temperature structures b) of a hot DA white dwarf model atmosphere with $T_{\rm eff}= 200~ 000$ K and $\log~g = 6.3$ with (solid line) and without (dashed line) Compton scattering taken into account.
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$\begin{figure} \par\includegraphics[width=7.3cm,height=10.5cm,clip]{5102fig2.eps} \end{figure}$	Figure 2: Spectra a) of the DA white dwarf HZ 43 model atmosphere with (solid line) and without (dashed line) Compton scattering using Method 1. Also shown are the spectra of the non-LTE model atmosphere (dotted line) and the spectra of non-LTE model atmosphere with Compton scattering (open circles). Run b) of Comptonisation parameter $Z_{\rm Compt}$ with wavelength (see Eq. (19)).
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$\begin{figure} \par\includegraphics[width=7.4cm,clip]{5102fig3.eps} \end{figure}$	Figure 3: Emergent X-ray spectra for a pure hydrogen model atmosphere appropriate for the parameters of HZ 43 computed for classical Thomson scattering (dashed) and Compton scattering (solid) using Method 2 (the method of Madej et al. 2004).
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$\begin{figure} \par\includegraphics[width=7.2cm,clip]{5102fig4.eps} \end{figure}$	Figure 4: The same as Fig. 2 but here for the DA white dwarf Sirius B LTE model atmosphere. The dotted line lies everywhere under the open circles (except for hydrogen lines).
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$\begin{figure} \par\includegraphics[width=7.2cm,clip]{5102fig5.eps} \end{figure}$	Figure 5: Spectra a) of the DA white dwarf $T_{\rm eff} = 100~ 000$ K model atmospheres with and without Compton scattering. Solid lines correspond to model with $\log~g=8.0$ , and dashed lines correspond to model with $\log~g = 6.0$ . Softer high energy tails correspond to models with Compton effect. Run b) of Comptonisation parameter $Z_{\rm Compt}$ with wavelength.
Open with DEXTER