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In this Symposium, researchers specializing in pulsation, rotation,
magnetic fields and stellar winds are brought together for the
first time in order to broaden our understanding of O and B stars.
Thanks to advances in digital spectroscopy, new types of pulsating
B stars have been discovered. The pulsations can be understood in
terms of the recent revision of metal opacities, but the effects of
rapid rotation and magnetic fields need further study. Observations
in the UV and X-ray regions demonstrate that many B and Be stars
show other activity, besides pulsation which is not yet understood.
The reason for the enhanced mass loss in Be stars is a question
which dominates the Symposium and which remains unanswered,
although it is surely to be found in activity at or near the
photosphere coupled with rotation. It is shown that the geometry of
the circumstellar envelopes around Be stars is indeed a flattened
disk as they can now be optically resolved. The variability of
radiatively-driven winds from O and B stars are likely related to
the rotation of the star. This underlines the central theme of the
book: that the various phenomena seen in these stars cannot be
studied in isolation.
In this Symposium, researchers specializing in pulsation, rotation,
magnetic fields and stellar winds are brought together for the
first time in order to broaden our understanding of O and B stars.
Thanks to advances in digital spectroscopy, new types of pulsating
B stars have been discovered. The pulsations can be understood in
terms of the recent revision of metal opacities, but the effects of
rapid rotation and magnetic fields need further study. Observations
in the UV and X-ray regions demonstrate that many B and Be stars
show other activity, besides pulsation which is not yet understood.
The reason for the enhanced mass loss in B stars is a question
which dominates the Symposium and which remains unanswered,
although it is surely to be found in activity at or near the
photosphere coupled with rotation. It is shown that the geometry of
the circumstellar envelopes around Be stars is indeed a flattened
disk as they can now be optically resolved. The variability of
radiatively-driven winds from O and B stars are likely related to
the rotation of the star. This underlines the central theme of the
book: that the various phenomena seen in these stars cannot be
studied in isolation.
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