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


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?".


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
  • 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