Astronomy and Astrophysics – Astronomy
Scientific paper
Feb 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984sci...223..777b&link_type=abstract
Science (ISSN 0036-8075), vol. 223, Feb. 24, 1984, p. 777-784.
Astronomy and Astrophysics
Astronomy
3
Chromosphere, Photosphere, Solar Temperature, Stellar Coronas, Stellar Radiation, Stellar Temperature, Energy Dissipation, Giant Stars, Hertzsprung-Russell Diagram, Main Sequence Stars, Radiative Transfer, Stellar Magnetic Fields, Supergiant Stars, X Ray Astronomy, X Ray Telescopes
Scientific paper
The increase in temperature outward from the surface of a stellar photosphere can be understood by looking at the local energy balance. The relatively high-density stellar photosphere is cooled effectively by radiative energy loss penetrating the optically thin corona. For the low-density chromosphere and corona, if the energy input cannot be balanced by radiative energy losses, the temperature will rise steeply, possibly up to 1 million degrees or more. Coronal heating and emission appear to be strongly influenced by magnetic fields, leading to large differences in X-ray emission for otherwise similar stars. Comparatively small variations are seen in the overall chromospheric emission of stars. Chromospheres are probably mainly heated by shock-wave energy dissipation, modified by magnetic fields.
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