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Mass Loss from Hot Stars: Main Sequence and Supergiant Stars

  • Conference paper
Mass Outflows from Stars and Galactic Nuclei

Part of the book series: Astrophysics and Space Science Library ((ASSL,volume 142))

Abstract

The determination of mass loss from early type stars by various methods is critically discussed. The reliability of the mass loss rates published in the literature is less than generally adopted.

The role of rotation on the mass loss is discussed in relation to the rapidly rotating B and Be-stars. The coupling between rotation and pulsation plays a major role in determining the structure and the variability of the winds.

The winds of stars near the Eddington limit are discussed in relation to the Luminous Blue Variables. Their winds are very different from those of normal supergiants, although both are due to radiation pressure. Small initial changes, possibly due to nonradial pulsations, can trigger large effects in the wind.

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Author information

Author notes

  1. Henny J. G. L. M. Lamers

    Present address: SRON Laboratory for Space Research, Beneluxlaan 21, 3527 HS, Utrecht, The Netherlands

Authors and Affiliations

  1. Joint Institute for Laboratory Astrophysics, University of Colorado Boulder, CO, 80309-0440, USA

    Henny J. G. L. M. Lamers

  2. National Bureau of Standards, University of Colorado Boulder, CO, 80309-0440, USA

    Henny J. G. L. M. Lamers

Authors
  1. Henny J. G. L. M. Lamers
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Editors and Affiliations

  1. Osservatorio Astronomico di Torino, Pino Torinese, Italy

    Luciana Bianchi

  2. ESA/VILSPA, IUE Groundstation, Madrid, Spain

    Roberto Gilmozzi

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© 1988 Kluwer Academic Publishers

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Lamers, H.J.G.L.M. (1988). Mass Loss from Hot Stars: Main Sequence and Supergiant Stars. In: Bianchi, L., Gilmozzi, R. (eds) Mass Outflows from Stars and Galactic Nuclei. Astrophysics and Space Science Library, vol 142. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-2941-8_4

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  • DOI: https://doi.org/10.1007/978-94-009-2941-8_4

  • Publisher Name: Springer, Dordrecht

  • Print ISBN: 978-94-010-7824-5

  • Online ISBN: 978-94-009-2941-8

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