All Figures

$\begin{figure} \par\includegraphics[width=8.4cm]{3540f1.ps} \end{figure}$ Figure 1: Unsharp-masked time-averaged white-light eclipse image processed by subtracting a 6 arcsec = 4300 km Gaussian convolution shown with contrast range $\Delta \ln I = 0.8\%$ . Dark and bright threads are probably flux tubes in current sheets.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm]{3540f2.ps} \end{figure}$ Figure 2: Log of scale-height function $\log_{10}\tilde\phi(r)$ for a solar polytrope atmosphere with $\Gamma =1.1$ and a potential magnetic field $\ell =2.33$ for different $\beta _{\rm s}$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm]{3540f3.ps} \end{figure}$ Figure 3: Relative flux-tube diameter $d(r)/d(r_{\rm s})$ in lower solar atmosphere with $\ell =2.33$ and $\beta _{\rm s}=5000$ for different polytrope adiabats $\Gamma$ ( upper panel), and with $\ell =2.33$ and $\Gamma =1.1$ for different $\beta _{\rm s}= 5$ , 50, $\dots$ 5.E5 ( lower panel). The arrow on each curve locates the most rapid temperature change for the model.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm]{3540f4.ps} \end{figure}$ Figure 4: Lower solar atmosphere $\log_{10}T(r)$ with $\ell =2.33$ and $\beta _{\rm s}=5000$ for different polytrope adiabats $\Gamma$ ( upper panel), and with $\ell =2.33$ and $\Gamma =1.1$ for different $\beta _{\rm s}$ ( lower panel), shown with the solar VAL A ( open circles) and F ( filled circles) atmospheres.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm]{3540f5.ps} \end{figure}$ Figure 5: Static solar corona T(r) for $\ell =.5$ , 1, 1.5, 2, and 2.5 (from top to bottom) shown with temperature from white-light intensity in the quiet equator ( filled circles), in SW ( crosses), and in SE ( open circles) streamers (Newkirk et al. 1970), and from line-width measurements ( dashed line) (Jarrett & von Klüber 1958).
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm]{3540f1.ps} \end{figure}$	Figure 1: Unsharp-masked time-averaged white-light eclipse image processed by subtracting a 6 arcsec = 4300 km Gaussian convolution shown with contrast range $\Delta \ln I = 0.8\%$ . Dark and bright threads are probably flux tubes in current sheets.
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$\begin{figure} \par\includegraphics[width=8.5cm]{3540f2.ps} \end{figure}$	Figure 2: Log of scale-height function $\log_{10}\tilde\phi(r)$ for a solar polytrope atmosphere with $\Gamma =1.1$ and a potential magnetic field $\ell =2.33$ for different $\beta _{\rm s}$ .
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.4cm]{3540f3.ps} \end{figure}$	Figure 3: Relative flux-tube diameter $d(r)/d(r_{\rm s})$ in lower solar atmosphere with $\ell =2.33$ and $\beta _{\rm s}=5000$ for different polytrope adiabats $\Gamma$ ( upper panel), and with $\ell =2.33$ and $\Gamma =1.1$ for different $\beta _{\rm s}= 5$ , 50, $\dots$ 5.E5 ( lower panel). The arrow on each curve locates the most rapid temperature change for the model.
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$\begin{figure} \par\includegraphics[width=8.5cm]{3540f4.ps} \end{figure}$	Figure 4: Lower solar atmosphere $\log_{10}T(r)$ with $\ell =2.33$ and $\beta _{\rm s}=5000$ for different polytrope adiabats $\Gamma$ ( upper panel), and with $\ell =2.33$ and $\Gamma =1.1$ for different $\beta _{\rm s}$ ( lower panel), shown with the solar VAL A ( open circles) and F ( filled circles) atmospheres.
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$\begin{figure} \par\includegraphics[width=8.4cm]{3540f5.ps} \end{figure}$	Figure 5: Static solar corona T(r) for $\ell =.5$ , 1, 1.5, 2, and 2.5 (from top to bottom) shown with temperature from white-light intensity in the quiet equator ( filled circles), in SW ( crosses), and in SE ( open circles) streamers (Newkirk et al. 1970), and from line-width measurements ( dashed line) (Jarrett & von Klüber 1958).
Open with DEXTER