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Radiation-accellerated ions in hot star winds: heating and “turbulence” effects

Published online by Cambridge University Press:  26 May 2016

E. Ya Vilkoviskij
E. Ya Vilkoviskij*
Affiliation:
V.G. Fessenkov Astrophysical Institute of the National Academy of Sciences, 480068 Almaty, Observatory AFI, Kazakhstan

Extract

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In the papers by Vilkoviskij (1981), Vilkoviskij and Tambovtzeva (1988) and Springmann and Pauldrach (1992) it was shown that ions can reach velocities relative to the wind plasma when the radiation pressure force exceeds the protons frictional force.

Type
7. OB Stellar Winds
Information
Symposium - International Astronomical Union , Volume 162: Pulsation, Rotation and Mass Loss in Early-Type Stars , 1994 , pp. 490 - 491
Copyright
Copyright © Kluwer 1994 

References

Springmann, U.V.E., Pauldrach, A.W.A.: 1992, Astronomy and Astrophysics 262, 515 Google Scholar
Vilkoviskij, E. Ya: 1981, Astrofisica (Sov) 17, 310 Google Scholar
Vilkoviskij, E. Ya., Tambovtzeva, L.V.: 1988, in: “Mass Outflows”, Bianchi, L., Gilmozzi, R. (eds.), p. 195 Google Scholar