| | [No title] (Site not responding. Last check: 2007-11-07) |
 | | The emission relation between $H\alpha$ and $H\beta$, which is determined by the total optical thickness, confirms earlier findings from spectra with a large sample of data points from six prominences. |
 | | Examples of the observed relation between this ratio and the $H\beta$ emission are given in Figs.~7 and 8 for the faint prominence at E/5S (cf., Fig.~3), and for the bright prominence W/28N (cf., Fig.~2). |
 | | Note that the emission ratio $Ca^+8542/H\beta$ is fairly constant over a large range of observed prominence emissions (particularly for the prominence at W/28N), thus confirming the spectro-photometric observations by Stellmacher and Wiehr (1997), and by De~Boer, Stellmacher and Wiehr (1998). |
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