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Pulsation and Mass Loss in Stars

Proceedings of a Workshop Held in Trieste, Italy, September 14–18, 1987

  • R. Stalio
  • L. A. Willson

Part of the Astrophysics and Space Science Library book series (ASSL, volume 148)

Table of contents

  1. Front Matter
    Pages i-xii
  2. Pulsation and Mass Loss from Cool Stars

    1. Front Matter
      Pages 1-1
    2. R. Hammer, M. Cuntz, M. Fracassini, L. E. Pasinetti Fracassini, E. G. Schmidt, T. J. Teays et al.
      Pages 73-79
  3. Pre-Main Sequence Objects

    1. Front Matter
      Pages 81-81
    2. Frank H. Shu, Susana Lizano, Fred C. Adams, Steven P. Ruden
      Pages 105-118
    3. Scott Kenyon, Lee Hartmann
      Pages 133-154
  4. Helio- and Astro- Seismology

  5. Pulsation and Mass Loss from Hot Stars

    1. Front Matter
      Pages 209-209
    2. John I. Castor, Stanley P. Owocki, George B. Rybicki
      Pages 229-249
    3. M. De Groot, L. Denizman, M. Hack, A. J. Willis, I. D. Howrath, L. J. Smith et al.
      Pages 275-281
  6. Pulsation, Mass Loss, and Stellar Evolution

    1. Front Matter
      Pages 283-283
  7. Meeting Summary: Comments by a Participant

    1. Front Matter
      Pages 313-313
    2. J. M. Marlborough
      Pages 315-319
  8. Back Matter
    Pages 321-336

About these proceedings

Introduction

Stellar mass loss is an essential part of the cycling of material from the interstellar medium into stars and back, and must be understood if we are to model processes on galactic to cosmological scales. The study of stellar winds and the effects of stellar mass loss has reached a particularly exciting stage where observational capabilities are increasingly able to provide interesting constraints on models and theories. Recent resu1ts from theoretical and observational work for both hot and cool stars with substantial winds have led to the suggestion that a combination of pulsation with other mechanisms makes for particularly efficient mass loss from stars. This provided the original motivation for the organization of this workshop. The conference was organized along relatively conventional lines according to the types of objects being scrutinized. However the true unity of the proceedings comes from the interplay of the mechanisms involved. For example, for the cool, luminous Mira variables, pulsation leads to shock waves that extend the atmosphere, enhancing dust formation; radiation pressure on dust drives the wind, cooling the atmosphere and in some cases suppressing the shocks. Similarly for the Be stars, both pulsation (in this case, non-radial) and radiation pressure (due to UV resonance lines) are expected to be important, and this expectation is at least qualitatively borne out by the observations.

Keywords

Accretion Variation interstellar matter stars stellar stellar evolution sun

Editors and affiliations

  • R. Stalio
    • 1
  • L. A. Willson
    • 2
  1. 1.Dipartimento di AstronomiaUniversità degli Studi di TriesteItaly
  2. 2.Physics DepartmentIowa State UniversityAmesUSA

Bibliographic information

  • DOI https://doi.org/10.1007/978-94-009-3029-2
  • Copyright Information Springer Science+Business Media B.V. 1988
  • Publisher Name Springer, Dordrecht
  • eBook Packages Springer Book Archive
  • Print ISBN 978-94-010-7861-0
  • Online ISBN 978-94-009-3029-2
  • Series Print ISSN 0067-0057
  • Buy this book on publisher's site