White-Light Emission of Solar Prominences

Details White-Light Emission of Solar Prominences White-Light Emission of Solar Prominences

May 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aspc..368..325j&link_type=abstract

The Physics of Chromospheric Plasmas ASP Conference Series, Vol. 368, Proceedings of the conference held 9-13 October, 2006 at t

Physics

1

Scientific paper

Using an extended grid of prominence models we compute the prominence white-light (WL) emission due to Thomson scattering and compare it with that in Hα. The ratio of the WL emission and the total emission can explain the color of prominences as observed during the total eclipses and can tell us whether the pink color of prominences is due to their intrinsic white-light emission or due to coronal contribution at the prominence location. We also show how this ratio depends on the prominence electron density, temperature and thickness.

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