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The warm wind model
Published online by Cambridge University Press: 14 August 2015
Abstract
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The analysis of the UV spectra of τ Sco (BO V) and ζ Pup (O4 f) resulted in the empirical warm wind model. In this model the presence of O5+ and N4+ ions in the envelopes of early type stars is explained by collisional ionization in a ‘warm’ envelope of T ≃ 2 105 K.
- Type
- Session 4: Panel Discussion on Stellar Wind Theories
- Information
- Symposium - International Astronomical Union , Volume 83: Mass Loss and Evolution of O-Type Stars , 1979 , pp. 191 - 199
- Copyright
- Copyright © Reidel 1979
References
Castor, J.I., Abbott, D.C., Klein, R.I.: 1976, in
Physique des Mouvements dans les Atmosphères Stellaires
, ed. Cayrel, R. and Steinberg, M., CNRS, Paris, p. 453.Google Scholar
Mewe, R., Heise, J., Gronenschild, E.H.B.M., Brinkman, A.C., Schrijver, J., den Boggende, A.J.F.: 1975, Astrophys. J. (Letters), 202, L67.Google Scholar
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