Energy balance in solar and stellar coronae.
Abstract
Methods for determining the energy balances in solar and stellar coronae are surveyed, and available results of such studies are presented for a range of late-type stars. The derivation of temperature and density structures from observed EUV and X-ray line fluxes is examined, and expressions for the terms in the energy balance equation expressing radiation losses and the net conductive flux are formulated in terms of atmospheric modeling parameters. Results of energy balance modeling are then illustrated for near main sequence stars including the sun (spectral type G2V) Procyon (F5 IV-V) and Epsilon Eri (K2 V), and for giants and supergiants including Beta Gem (K0 III) and Alpha Tau (K5 III). It is noted that the main sequence stars have hot coronae with thermal conduction important, while the giants and supergiants have either hot or cool coronae depending on the surface gravity and the presence of a strong stellar wind.
- Publication:
-
Solar Phenomena in Stars and Stellar Systems
- Pub Date:
- 1981
- Bibcode:
- 1981ASIC...68..199J
- Keywords:
-
- Electron Density (Concentration);
- Energy Budgets;
- Late Stars;
- Main Sequence Stars;
- Solar Corona;
- Stellar Coronas;
- Atmospheric Temperature;
- Electron Scattering;
- Flux Density;
- Stellar Atmospheres;
- Stellar Winds;
- Astrophysics;
- Stellar Coronae:Models