$\begin{figure} \par\includegraphics[width=18cm,clip]{Hh311_f1} \end{figure}$ Figure 1: HETGS spectrum and a parameterized best-fit model of TW Hya (summed plus- and minus orders); line letter designations refer to the line parameters given in Table 1.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{Hh311_f2} \end{figure}$ Figure 2: Density dependence of the Fe XVII line ratio $\lambda \lambda 17.10/17.05$ predicted by APEC and M.F. Gu compared with 18 coronal measurements and TW Hya; plasma densities are derived from Ne IX f/i ratios.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{Hh311_f3} \end{figure}$ Figure 3: Theoretical predictions of Ly $\beta$ /Ly $\alpha$ ratio as a function of temperature for O VIII and measurements of TW Hya compared with stellar measurements (temperatures from O VIII/O VII line ratios); shaded areas are predictions for values of $N_{\rm H}<4\times 10^{20}$ cm^-2.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{Hh311_f4} \end{figure}$ Figure 4: Area vs. density $N_{\rm e}$ from the requirement optical depth $\tau < 1$ ; area values for surface filling factors are indicated.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=18cm,clip]{Hh311_f1} \end{figure}$	Figure 1: HETGS spectrum and a parameterized best-fit model of TW Hya (summed plus- and minus orders); line letter designations refer to the line parameters given in Table 1.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{Hh311_f2} \end{figure}$	Figure 2: Density dependence of the Fe XVII line ratio $\lambda \lambda 17.10/17.05$ predicted by APEC and M.F. Gu compared with 18 coronal measurements and TW Hya; plasma densities are derived from Ne IX f/i ratios.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{Hh311_f3} \end{figure}$	Figure 3: Theoretical predictions of Ly $\beta$ /Ly $\alpha$ ratio as a function of temperature for O VIII and measurements of TW Hya compared with stellar measurements (temperatures from O VIII/O VII line ratios); shaded areas are predictions for values of $N_{\rm H}<4\times 10^{20}$ cm^-2.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{Hh311_f4} \end{figure}$	Figure 4: Area vs. density $N_{\rm e}$ from the requirement optical depth $\tau < 1$ ; area values for surface filling factors are indicated.
Open with DEXTER