Outer atmospheres of cool stars. IV - A discussion of cool stellar wind models

Details Outer atmospheres of cool stars. IV - A discussion of cool stellar wind models Outer atmospheres of cool stars. IV - A discussion of cool stellar wind models

Jan 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980apj...235..519h&link_type=abstract

Astrophysical Journal, Part 1, vol. 235, Jan. 15, 1980, p. 519-533.

Astronomy and Astrophysics

Astrophysics

35

Chromosphere, Cool Stars, Late Stars, Stellar Models, Stellar Temperature, Stellar Winds, Coronas, Flow Equations, Hertzsprung-Russell Diagram, Magnetohydrodynamic Waves, Radiation Pressure, Stellar Mass Ejection

Scientific paper

Possible wind models for late-type stars which appear not to have hot coronae and transition regions are investigated; taking Arcturus and the prototypical star, models with T less than approximately 20,000 K are considered, and solutions with mass loss rates of 10 to the -9th solar masses per year are sought. The radiation pressure of L-alpha resonance scattering can exceed the force of gravity in the chromosphere and initiate a net outflow, but is insufficient to sustain a wind, except perhaps in the presence of an additional momentum input term such as Alfven wave pressure. It is concluded that L-alpha radiation-pressure-initiated winds can occur in stars to the right of the Linsky-Haisch dividing line in the H-R diagram between stars with and without transition regions and presumably hot coronae, and that the existence of these winds may explain energetically the absence of hot coronae in these stars.

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