Abstract
Main sequence OB-stars are useful for testing X-ray source models, because the mass loss rates are low as compared to those of the OB supergiants and the Of stars hence the winds are optically thin at nearly all frequencies. We are therefore able to detect the emission from all parts of the outer atmosphere and not be concerned that some source regions are attenuated from our view. The analyses of the X-ray emission and the ultraviolet line profiles are relatively straight-forward.
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© 1987 D. Reidel Publishing Company, Dordrecht, Holland
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Cassinelli, J.P. (1987). The X-Ray Emission of TAU SCO, BO V, and the Problems Posed for Embedded Shock Models. In: Lamers, H.J.G.L.M., De Loore, C.W.H. (eds) Instabilities in Luminous Early Type Stars. Astrophysics and Space Science Library, vol 136. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-3901-1_31
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DOI: https://doi.org/10.1007/978-94-009-3901-1_31
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