A Prominence Model Based on Spectral Observations
Abstract
Intensities and profiles of the Hα, Hβ, Hγ, K, and D3 lines are measured in a solar prominence. From the profiles of these lines we estimate T = 6400 K and υt = 5.7 km s−1. We construct a simple isothermal model which explains the Hα intensity and profile for an assumed total particle density nT = 3 × 1011 cm−3, and a filling factor, α = 1/6.
- Publication:
-
Solar Physics
- Pub Date:
- November 1979
- DOI:
- 10.1007/BF00151126
- Bibcode:
- 1979SoPh...64..177F
- Keywords:
-
- 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;
- Solar Physics;
- Energy Loss;
- Particle Density;
- Radiative Energy;
- Filling Factor;
- Isothermal Model