A prominence model based on spectral observations

Details A prominence model based on spectral observations A prominence model based on spectral observations

Nov 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979soph...64..177f&link_type=abstract

Solar Physics, vol. 64, Nov. 1979, p. 177-186.

Physics

8

Atmospheric Models, Line Spectra, Solar Prominences, Solar Spectra, D Lines, H Alpha Line, H Beta Line, H Gamma Line, K Lines, Particle Density (Concentration), Radiative Transfer, Spectroheliographs, Spectrum Analysis

Scientific paper

Intensities and profiles of the H-alpha, H-beta, H-gamma, K, and D3 lines are measured in a solar prominence. From the profiles of these lines T = 6400 K and vt = 5.7 km/s were estimated. A simple isothermal model which explains the H-alpha intensity and profile for an assumed total particle density of 3 x 10 to the 11th per cu cm and a filling factor of alpha = 1/6 was constructed. From this model it is found that the source function is nearly constant through the prominence. It is estimated that the radiative energy loss at the center of the prominence is of the order of 10 to the 7th erg/s/g.

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