Heating of stellar chromospheres when magnetic fields are present

Details Heating of stellar chromospheres when magnetic fields are present Heating of stellar chromospheres when magnetic fields are present

Feb 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982a%26a...106....9u&link_type=abstract

Astronomy and Astrophysics, vol. 106, no. 1, Feb. 1982, p. 9-13. Research supported by the Deutsche Forschungsgemeinschaft and

Computer Science

Sound

60

Chromosphere, Gas Heating, Magnesium, Oso-8, Stellar Magnetic Fields, Stellar Models, Stellar Spectra, Emission Spectra, Line Spectra, Magnetohydrodynamic Waves, Shock Waves, Sound Waves

Scientific paper

Constraints on possible mechanisms of chromospheric heating are derived from recent, semi-empirical solar models, OSO-8 observations, and the stellar Mg II emission-line fluxes of Basri and Linsky (1979). It is shown that the observational facts are best satisfied by a scenario in which non-magnetic regions are heated by acoustic shock waves, while magnetic regions are heated by slow-mode shock waves. For the case of the high chromosphere, however, this mechanism must be either supplemented or replaced by such alternatives as Alfven wave heating.

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