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The warm wind model
Published online by Cambridge University Press: 14 August 2015
Abstract
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