Lyalpha radiation from coronal transients
Abstract
The intensity and profile of the Lyman alpha spectral line expected from the extended coronal plasma evolving during a coronal transient, when observed in the plane of the sky in the range of heliocentric distance 1.5 to 4 solar radii, are calculated. The numerical values of temperature, density and outflow speed inside the coronal transient are those determined by Wu and Wang under the assumption of a single fluid, three dimensional, time dependent magnetohydrodynamic model of the outer solar atmosphere. The dependence of the Lyman alpha line on the physical parameters of the examined structure is discussed. These results may help in preparing and interpreting UVCS/SOHO (Ultraviolet Coronagraph/Solar and Heliospheric Observatory) observations of coronal transients.
- Publication:
-
Coronal Streamers, Coronal Loops, and Coronal and Solar Wind Composition
- Pub Date:
- November 1992
- Bibcode:
- 1992ESASP.348..105S
- Keywords:
-
- Brightness;
- Lyman Alpha Radiation;
- Radiation Distribution;
- Soho Mission;
- Solar Corona;
- Solar Radiation;
- Solar Wind;
- Surges;
- Astronomical Models;
- Line Spectra;
- Magnetohydrodynamics;
- Mathematical Models;
- Solar Atmosphere;
- Ultraviolet Radiation;
- Solar Physics