Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{emis_theo.ps} \end{figure}$ Figure 1: Theoretical line fluxes for a cosmic abundance plasma for H-like and He-like resonance lines for C (solid lines), N (dotted lines), O (short-dashed lines), Ne (dash-dotted lines), Mg (dash-triple dotted lines), and Si (long-dashed lines) as calculated with the MEKAL code. Note, that for all elements the Ly $_{\alpha }$ lines are stronger than the He-like resonance lines.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{lyrat} \end{figure}$ Figure 2: Theoretical line flux ratios of H-like by He-like resonance lines for C, N, O, Ne, Mg, and Si in comparison with the measured ratios for Algol, Capella, and Procyon.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{dem.ps} \end{figure}$ Figure 3: Best fit differential emission measure distributions with fourth-order Chebyshev polynomials and temperatures $T_{\rm max} = 20$ MK, 30 MK, 40 MK, and 50 MK; only the choices $T_{\rm max} = 30$ MK and $T_{\rm max} = 40$ MK yield acceptable fits to the Chandra LETGS data.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{demord.ps} \end{figure}$ Figure 4: Best fit differential emission measure distributions with Chebyshev polynomials with ( $T_{\rm max} = 30$ MK, M=4; dashed curve), ( $T_{\rm max} = 40$ MK, M=4; solid curve), and ( $T_{\rm max}=50$ MK, M=7; dotted curve). All parameter choices yield acceptable fits to the Chandra LETGS line ratio data, the higher temperature yield better continuum values.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{cfit.eps} \end{figure}$ Figure 5: Chandra LETGS spectrum for Algol binned in wavelength bins with a width of TBD Å (dots) and best fit differential emission measure model continuum for M=4 and $T_{\rm max} = 40$ MK (solid line); dashed curves indicate a 15% systematic uncertainty in effective instrument areas. Note that the continuum has been calculated from the abundances actually derived for Algol.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{gass.ps} \end{figure}$ Figure 6: Best fit differential emission measure distribution derived from Eq. (40) (solid curve) compared to DEM distributions derived from fourth order Chebyshev polynomials with $T_{\rm max} = 30$ MK and $T_{\rm max} = 40$ MK.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{emis_theo.ps} \end{figure}$	Figure 1: Theoretical line fluxes for a cosmic abundance plasma for H-like and He-like resonance lines for C (solid lines), N (dotted lines), O (short-dashed lines), Ne (dash-dotted lines), Mg (dash-triple dotted lines), and Si (long-dashed lines) as calculated with the MEKAL code. Note, that for all elements the Ly $_{\alpha }$ lines are stronger than the He-like resonance lines.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{lyrat} \end{figure}$	Figure 2: Theoretical line flux ratios of H-like by He-like resonance lines for C, N, O, Ne, Mg, and Si in comparison with the measured ratios for Algol, Capella, and Procyon.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{dem.ps} \end{figure}$	Figure 3: Best fit differential emission measure distributions with fourth-order Chebyshev polynomials and temperatures $T_{\rm max} = 20$ MK, 30 MK, 40 MK, and 50 MK; only the choices $T_{\rm max} = 30$ MK and $T_{\rm max} = 40$ MK yield acceptable fits to the Chandra LETGS data.
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$\begin{figure} \par\includegraphics[width=8.1cm,clip]{demord.ps} \end{figure}$	Figure 4: Best fit differential emission measure distributions with Chebyshev polynomials with ( $T_{\rm max} = 30$ MK, M=4; dashed curve), ( $T_{\rm max} = 40$ MK, M=4; solid curve), and ( $T_{\rm max}=50$ MK, M=7; dotted curve). All parameter choices yield acceptable fits to the Chandra LETGS line ratio data, the higher temperature yield better continuum values.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{cfit.eps} \end{figure}$	Figure 5: Chandra LETGS spectrum for Algol binned in wavelength bins with a width of TBD Å (dots) and best fit differential emission measure model continuum for M=4 and $T_{\rm max} = 40$ MK (solid line); dashed curves indicate a 15% systematic uncertainty in effective instrument areas. Note that the continuum has been calculated from the abundances actually derived for Algol.
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$\begin{figure} \par\includegraphics[width=7.9cm,clip]{gass.ps} \end{figure}$	Figure 6: Best fit differential emission measure distribution derived from Eq. (40) (solid curve) compared to DEM distributions derived from fourth order Chebyshev polynomials with $T_{\rm max} = 30$ MK and $T_{\rm max} = 40$ MK.
Open with DEXTER