Astronomy and Astrophysics – Astrophysics
Scientific paper
Apr 1981
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981afz....17..309v&link_type=abstract
(Astrofizika, vol. 17, Apr.-June 1981, p. 309-315.) Astrophysics, vol. 17, no. 2, Oct. 1981, p. 170-174. Translation.
Astronomy and Astrophysics
Astrophysics
4
Early Stars, Plasma Heating, Radiation Pressure, Stellar Winds, Ion Motion, Kinetic Heating, Plasma Temperature, Stellar Envelopes
Scientific paper
It has heretofore been assumed that the source of stellar wind heating is due to the dissipation of gas-dynamic perturbations, excited by the high radiation flux of the star (Hearn, 1975). A different mechanism, called the kinetic mechanism, is proposed to account for the heating of star envelopes with high radiation pressure. Radiation pressure causes the element ions of the type C III to move with high velocities (of the order 100,000,000 cm/sec) relative to the stellar wind plasma. This results in a heating of the outer regions of the stellar wind to a temperature of about 200,000 K. This heating leads to a change in the flow velocity, and thus in the plasma parameters, but only when the critical conditions are reached. The conditions under which this heating mechanism operates are specified.
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