Physics
Scientific paper
Mar 1988
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988soph..114...47k&link_type=abstract
Solar Physics, Volume 114, Issue 1, pp.47-64
Physics
Scientific paper
We have calculated the emission spectra of hydrogen and sodium atoms in the cool part of prominence models which satisfy simultaneously the constraints of radiative transfer, statistical equilibrium and charge-particle conservations. In the considered range of our model parameters, emission strengths of Hα and Na i D lines increase with the temperature and the total number density. Low-pressure models raise the ionization rate highly but yield very weak Na i D line intensities, since these model prominences contain small amounts of free electrons and sodium atoms which have a deep relation with the formation of sodium lines. We find that sodium D lines should be emitted in the high pressure region of prominences, and that their intensities are difficult to attain in the cool core of any model prominence with a temperature as low as 4000 K. In order to explain consistently the spectral emissions of Hα and Na i D lines observed in quiescent prominences, a total number density higher than 4 x 1011 cm-3 and a temperature over 5000 K are required at least in the cool part of prominences.
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