Astron. Astrophys. 344, 205-210 (1999)

On the decoupling and reaccretion of low density, line-driven winds

John M. Porter and Barry A. Skouza

Astrophysics Research Institute, Liverpool John Moores University, Twelve Quays House, Egerton Wharf, Birkenhead, L41 1LD, UK (jmp@astro.livjm.ac.uk)

Received 7 August 1998 / Accepted 7 January 1999

Abstract

The flow generated by low-density radiatively driven winds which decouple their gas and radiation fields is discussed. In particular we concentrate on flow which is still bound to the star and can therefore reaccrete. The wind decelerates after decoupling and eventually stalls. A shell of gas is generated, and we find that this shell is unstable and contracts back to the star with periods of hours to days.

We find that the pulsating shells may be difficult to observe, as their emission is variable and the maximum emission at (of of the continuum) occurs over a small fraction of the shell cycle.

Key words: hydrodynamics stars: circumstellar matter stars: early-type stars: mass-loss

This article contains no SIMBAD objects.

Contents

• 1. Introduction
• 2. Decoupling physics
• 3. Results
  • 3.1. Analytic considerations
  • 3.2. Numerical hydrodynamic modelling
• 4. Observable signatures
• 5. Discussion and conclusions
• Acknowledgements
• References

© European Southern Observatory (ESO) 1999

Online publication: March 10, 1999
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