White-Light Emission of Solar Prominences

Using an extended grid of prominence models we compute the prominence white-light emission and compare it with the H-alpha one. The ratio of these two emissions 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. Finally, we use recent eclipse observations from 29 March 2006 to check our model results.