Hostname: page-component-cd9895bd7-hc48f Total loading time: 0 Render date: 2024-12-25T15:38:30.550Z Has data issue: false hasContentIssue false
  • English
  • Français

Thermal and Continuum Driven Convection in B-Stars

Published online by Cambridge University Press:  12 April 2016

George Driver Nelson
George Driver Nelson*
Affiliation:
CODE CB, Johnson Space Center, Houston, Texas, 77058

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Two regions of convective instability are present in the photosphere of a typical B-star (Teff = 30,000 K Log g = 4.0). One is the usual thermal instability caused by the helium ionization. The other is driven by the continuum radiation pressure in a thermally stable layer. Mixing length and anelastic modal representations of these unstable regions show that the rapid radiative cooling of temperature fluctuations limits the velocities to an amplitude of a few meters per second, much too small to account for the observed line broadening and asymmetries.

Type
1. The Pyhsical Origin of Turbulence
Information
International Astronomical Union Colloquium , Volume 51: Stellar Turbulence , 1980 , pp. 16
Copyright
Copyright © Springer-Verlag 1980