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Dust formation as a diagnostic of Wolf-Rayet winds

Published online by Cambridge University Press:  26 May 2016

Peredur M. Williams ,
Karel A. van der Hucht ,
Patrick W. Morris  and
Fred Marang
Peredur M. Williams
Affiliation:
Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, Scotland, UK
Karel A. van der Hucht
Affiliation:
SRON Nationaal Instituut voor Ruimteonderzoek, Sorbonnelaan 2, NL-3584 CA Utrecht, Nederland
Patrick W. Morris
Affiliation:
SIRTF Science Center, IPAC, California Institute of Technology, Pasadena, CA 91125, U.S.A.
Fred Marang
Affiliation:
South African Astronomical Observatory, P.O. Box 9, Observatory, 7935, South Africa

Abstract

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Dust formation by Wolf-Rayet stars is a powerful diagnostic of exceptional activity in their winds. Observed behaviour ranges from stars which make dust continually (e.g., WR 104, WC9d+B0.5V) to those which make dust for short episodes at periodic intervals (e.g., WR 140, WC7pd+04-5). In both examples, dust formation is related to colliding WR and OB stellar winds in binary orbits. We have been using IR photometry primarily from the SAAO and ESO and spectroscopy with ISO-sws to investigate systems having intermediate properties (WR 98a, WC8-9vd+?) or more complex behaviour (WR 48a, WC8ed+?).

Information

Type
Part 1. Atmospheres of Massive Stars
Information
Symposium - International Astronomical Union , Volume 212: A Massive Star Odyssey: From Main Sequence to Supernova , 2003 , pp. 115 - 120
Copyright
Copyright © Astronomical Society of the Pacific 2003 

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