Stellar coronae.
Abstract
The physics of stellar coronae are discussed on the basis of recent observations of the solar corona and stellar X-ray emission. The standard scenario of stellar coronal formation and dynamics, which predicts that the level of coronal emission should follow the level of acoustic flux generation rather than rotation rate and that mass loss will vary with coronal activity level, is outlined. Results are then reviewed of solar observations, which indicate that high mass loss rates are associated with regions of low activity and that coronal activity levels correlate with surface magnetic fields, and of Einstein X-ray observations, which have demonstrated that X-ray emission is associated with stars throughout the H-R diagram. On the basis of these observations, a model of stellar corona formation is suggested in which stellar magnetic fields play the key role in determining the level of coronal emission, and the modulation of the surface magnetic flux level and the level of surface magnetic field stressing essentially determine the variation of mean coronal activity in the H-R diagram
- Publication:
-
Highlights of Astronomy
- Pub Date:
- 1980
- Bibcode:
- 1980HiA.....5..419V
- Keywords:
-
- Main Sequence Stars;
- Stellar Coronas;
- Stellar Evolution;
- Stellar Spectra;
- X Ray Sources;
- Astronomical Observatories;
- Hertzsprung-Russell Diagram;
- Stellar Atmospheres;
- Stellar Magnetic Fields;
- Stellar Mass Ejection;
- Astronomy;
- Magnetic Fields:Stellar Coronae;
- Solar Corona:Heating;
- Stellar Coronae:Formation;
- Stellar Coronae:X Rays