Coronal activity in late-type main-sequence stars

Details Coronal activity in late-type main-sequence stars Coronal activity in late-type main-sequence stars

Dec 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...335..892s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 335, Dec. 15, 1988, p. 892-906. Research supported by NSERC and Polska Akad

Astronomy and Astrophysics

Astrophysics

13

Late Stars, Magnetic Stars, Magnetohydrodynamic Waves, Main Sequence Stars, Stellar Coronas, F Stars, G Stars, K Stars, Kinetic Energy, Specific Heat

Scientific paper

A method of taking into account the back-reaction of mechanical waves on the turbulent medium generating these waves is suggested. With this feedback included, Alfvén wave fluxes for late-type main-sequence stars are computed and compared with observed coronal radiative losses. From this comparison the filling factor describing the coverage of stellar surface with strong magnetic tubes is determined. The filling factor varies between 10-1 and 10-5 and correlates well with the Rossby number and observed magnetic fields. The relation between the filling factor and the Rossby number is derived. No evidence is found for a sudden drop of coronal activity among late M stars.

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