Astronomy and Astrophysics – Astrophysics
Scientific paper
Feb 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986apj...301..297b&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 301, Feb. 1, 1986, p. 297-301.
Astronomy and Astrophysics
Astrophysics
11
Boundary Layers, Chromosphere, Stellar Coronas, Stellar Temperature, Magnetohydrodynamic Waves, Shock Wave Attenuation, Wave Attenuation
Scientific paper
It is found that, for stars with low gravitational acceleration, transition layers between chromosphere and corona cannot form, because the chromospheres are so extended that the mechanical energy flux decreases faster than the square of the electron density. There is not enough flux left to lead to a steep temperature increase in the transition layer and corona. If the disipation length lambda for the mechanical energy flux is the same for all stars, the boundary line for transition layers would be expected to coincide with a line of g = const in the H-R diagram. The numerial value for this g depends on the dissipation length. A comparison with the observed boundary line shows that the dissipation length is not the same for all stars but increases roughly as (Teff/g) exp 0.93.
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