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Time-resolved optical-UV spectroscopy of colliding wind effects

Published online by Cambridge University Press:  25 May 2016

Anthony F.J. Moffat
Anthony F.J. Moffat*
Affiliation:
Département de physique, Université de Montréal, C.P. 6128, Succ. Centre-Ville, Montréal, Qc H3C 3J7, Canada

Abstract

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It is in the ultraviolet-optical domain where the strongest known emission lines arise in hot star winds. In the case of hot-star binaries, culminating in the relatively common, strong-wind WR+O systems, similar line-emission is seen in the cooling flows downstream from the highly compressed, X-ray emitting heads of the bow shock regions produced when the two winds collide. Time-resolved UV-optical spectroscopy of these flows around a complete orbit can provide important constraints not only on the colliding wind process itself, but also on the winds and the orbit. Spectroscopic wind-wind collision effects have now been seen in every relatively close WR+O system (P ≲ 100 d) that has been adequately observed so far.

Type
Part 3. Interaction of Wolf-Rayet stars and other hot massive stars with their environment: colliding winds and ring nebulae
Information
Symposium - International Astronomical Union , Volume 193: Wolf-Rayet Phenomena in Massive Stars and Starburst Galaxies , 1999 , pp. 278 - 288
Copyright
Copyright © Astronomical Society of the Pacific 1999 

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