Theory of stellar coronae - an interpretation of X-ray emission from non-degenerate stellar sources

Details Theory of stellar coronae - an interpretation of X-ray emission from non-degenerate stellar sources Theory of stellar coronae - an interpretation of X-ray emission from non-degenerate stellar sources

Nov 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981assl...87...19l&link_type=abstract

In: X-ray astronomy with the Einstein satellite; Proceedings of the Meeting, Cambridge, MA, January 28-30, 1980. (A82-33476 16-9

Astronomy and Astrophysics

Astronomy

4

Atmospheric Heating, Solar Corona, Stellar Magnetic Fields, Stellar Radiation, Stellar Rotation, X Ray Sources, Binary Stars, Convective Flow, Heao 2, Stellar Structure, Stellar Winds

Scientific paper

It is shown that the acoustic wave heating theory of stellar coronae explains neither Einstein Observatory coronae data nor previous UV and X-ray observations of the sun and other stars, on the evidence of data implying that magnetic fields, stellar rotation rates and convection zone parameters figure in the determination of coronal heating. Einstein Observatory results suggest that O-type star coronae are heated by the interaction of turbulent stellar winds with slowly-decaying primordial magnetic fields or by radiative instabilities in the flow. The apparent absence of coronae in Ap stars is due to the stability of atmospheres in which even weak convection is suppressed by the strong field. Dynamo action is implicated in some normal A-type stars and in F- and later-type dwarfs. Coronal characteristics of dMe and dM stars, close binaries, and K- and M-type giants are also considered.

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