The Wind of P Cygni

  • J. Puls
  • A. W. A. Pauldrach
  • R. P. Kudritzki
Conference paper
Part of the Astrophysics and Space Science Library book series (ASSL, volume 157)

Abstract

The stationary features of the wind of P Cygni are considerably different from those of ‘normal’ supergiant winds with comparable luminosity. In contrast to such winds, which are generally accepted to be driven by radiation pressure, P Cygni’s mass-loss rate is higher by a factor of 5, the terminal velocity is higher by a factor of 10, and the velocity law itself is much flatter than would be expected from a first glance at glance at typical scaling relations. However, these relations depend crucially and non- linearly on the star′s distance from the Eddington limit, which for P Cyg is very small (see below). Here we investigate whether the acceleration mechanism of P Cygni’s wind can also be explained by line pressure and to what extent self-consistent wind models represent the observed quantities (especially the IR energy distribution).

Keywords

Radiation Pressure Terminal Velocity Acceleration Mechanism Line Force Stellar Parameter 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

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Copyright information

© Kluwer Academic Publishers 1989

Authors and Affiliations

  • J. Puls
    • 1
  • A. W. A. Pauldrach
    • 1
  • R. P. Kudritzki
    • 1
  1. 1.Institut f. Astronomie & AstrophysikUniversität München, ScheinerstraβeMünchen 80Germany

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