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)


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).


Radiation Pressure Terminal Velocity Acceleration Mechanism Line Force Stellar Parameter 
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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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