Pulsation, Rotation and Mass Loss in Early-Type Stars

Proceedings of the 162nd Symposium of the International Astronomical Union, Held in Antibes-Juan-Les-Pins, France, October 5–8, 1993

  • Luis A. Balona
  • Huib F. Henrichs
  • Jean Michel Le Contel
Conference proceedings

Table of contents

  1. Front Matter
    Pages i-xxii
  2. Pulsation and Rotation

    1. Front Matter
      Pages 1-1
    2. Mikolaj Jerzykiewicz
      Pages 3-14
    3. H. Cugier, W. A. Dziembowski, A. A. Pamyatnykh
      Pages 15-16
    4. H. Cugier, A. Pigulski, G. Polubek, R. Monier
      Pages 17-18
    5. P. Moskalik, J. R. Buchler
      Pages 19-20
    6. E. Chapellier, J. C. Valtier
      Pages 23-24
    7. J. C. Valtier, E. Chapellier, J. M. Le Contel
      Pages 25-26
    8. C. Waelkens, H. van Winckel, K. de Mey
      Pages 27-28
    9. H. Kjeldsen, D. Baade
      Pages 29-30
    10. Salvador González Bedolla
      Pages 31-32
    11. L. Huang, Z. Guo, J. Hao, J. R. Percy, M. S. Fieldus, R. Fried et al.
      Pages 33-36
    12. H. Sadsaoud, D. Le Contel, E. Chapellier, S. González-Bedolla, J. M. Le Contel
      Pages 39-40
    13. P. North, S. Paltani
      Pages 41-42
    14. R. Kuschnig, W. W. Weiss, N. Piskounov, T. Ryabchikova, T. J. Kreidl, M. Alvarez et al.
      Pages 43-46
    15. E. Solano, J. Fernley
      Pages 47-48
    16. Søren Frandsen
      Pages 49-50
    17. Nancy Remage Evans
      Pages 51-52

About these proceedings

Introduction

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.

Keywords

LOPES photometry spectroscopy star stellar

Editors and affiliations

  • Luis A. Balona
    • 1
  • Huib F. Henrichs
    • 2
  • Jean Michel Le Contel
    • 3
  1. 1.South African Astronomical ObservatoryCape TownSouth Africa
  2. 2.Astronomical InstituteUniversity of AmsterdamAmsterdamThe Netherlands
  3. 3.Observatoire de la Côte d’AzurNiceFrance

Bibliographic information

  • DOI https://doi.org/10.1007/978-94-011-1030-3
  • Copyright Information International Astronomical Union 1994
  • Publisher Name Springer, Dordrecht
  • eBook Packages Springer Book Archive
  • Print ISBN 978-0-7923-3045-5
  • Online ISBN 978-94-011-1030-3
  • About this book
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