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Mass Loss from Red Giants

Proceedings of a Conference held at the University of California at Los Angeles, U.S.A., June 20–21, 1984

  • Mark Morris
  • Ben Zuckerman
Conference proceedings

Part of the Astrophysics and Space Science Library book series (ASSL, volume 117)

Table of contents

  1. Front Matter
    Pages i-xvi
  2. Leo Goldberg
    Pages 21-27
  3. A. K. Dupree, L. Hartmann, G. H. Smith, E. H. Avrett
    Pages 29-30
  4. Jacques M. Beckers
    Pages 57-61
  5. R. Sahai, P. G. Wannier
    Pages 81-82
  6. Kenneth H. Hinkle
    Pages 85-86
  7. W. Schutte, A. G. G. M. Tielens
    Pages 87-93
  8. Steven Beckwith
    Pages 95-113
  9. Michael L. Cobb, John D. Fix
    Pages 115-116
  10. R. Sahai, Alwyn Wootten, R. E. S. Clegg
    Pages 151-152
  11. J. H. Bieging, B. Chapman, W. J. Welch
    Pages 155-156
  12. G. R. Knapp, Kar Man Chang, Mark Morris
    Pages 159-159
  13. C. R. Masson, K. W. Cheung, G. L. Berge, M. J. Claussen, G. M. Heiligman, R. B. Leighton et al.
    Pages 165-167
  14. Harley A. Thronson Jr., John Bally
    Pages 169-170
  15. G. R. Knapp
    Pages 171-173
  16. M. J. Claussen, R. Sahai
    Pages 185-186
  17. D. Engels, H. J. Habing, F. M. Olnon, J. Schmid-Burgk, C. M. Walmsley
    Pages 211-212
  18. Anneila I. Sargent, Boudewijn Baud
    Pages 213-214
  19. J. Herman
    Pages 215-220
  20. P. R. Jewell, C. Henkel, C. M. Walmsley, T. L. Wilson, L. E. Snyder, D. Engels
    Pages 227-228
  21. Thomas E. Holzer, Keith B. MacGregor
    Pages 229-255
  22. M. J. Drinkwater, P. R. Wood
    Pages 257-260
  23. S. R. Sreenivasan, W. J. F. Wilson
    Pages 261-263
  24. Gordon C. Augason
    Pages 265-267
  25. A. G. G. M. Tielens, M. Werner, R. Capps
    Pages 305-307
  26. H. Benton Ellis Jr., Michael W. Werner
    Pages 309-310
  27. Rieu Q. Nguyen, D. Graham, V. Bujarrabal
    Pages 311-312
  28. Peter Goldreich
    Pages 313-315
  29. Back Matter
    Pages 317-320

About these proceedings

Introduction

Red giant and supergiant stars have long been favorites of professional 6 and amateur astronomers. These enormous stars emit up to 10 times more energy than the Sun and, so, are easy to study. Some of them, specifically the pulsating long-period variables, significantly change their size, brightness, and color within about a year, a time scale of interest to a single human being. Some aspects of the study of red giant stars are similar to the study of pre-main-sequence stars. For example, optical astronomy gives us a tantalizing glimpse of star forming regions but to really investi­ gate young stars and protostars requires infrared and radio astronomy. The same is true of post-main-sequence stars that are losing mass. Optical astronomers can measure the atomic component of winds from red giant stars that are undergoing mass loss at modest rates 6 (M $ 10- M9/yr.). But to see dust grains and molecules properly, 5 especially in stars with truly large mass loss rates, ~ 10- M9/yr, one requires IR and radio astronomy. As this stage of copious mass loss only lasts for ~105 years one might be tempted to ask, "who cares?".

Keywords

LOPES Variation astronomy gravity interferometry optical interferometry photometry planet radio astronomy spectroscopy star stars stellar sun telescope

Editors and affiliations

  • Mark Morris
    • 1
  • Ben Zuckerman
    • 1
  1. 1.Department of AstronomyUCLALos AngelesUSA

Bibliographic information

  • DOI https://doi.org/10.1007/978-94-009-5428-1
  • Copyright Information Springer Science+Business Media B.V. 1985
  • Publisher Name Springer, Dordrecht
  • eBook Packages Springer Book Archive
  • Print ISBN 978-94-010-8896-1
  • Online ISBN 978-94-009-5428-1
  • Series Print ISSN 0067-0057
  • Buy this book on publisher's site
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