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Time-resolved optical-UV spectroscopy of colliding wind effects

  • Anthony F.J. Moffat (a1)

Abstract

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.

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References

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Time-resolved optical-UV spectroscopy of colliding wind effects

  • Anthony F.J. Moffat (a1)

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