Hostname: page-component-745bb68f8f-kw2vx Total loading time: 0 Render date: 2025-01-13T18:45:03.924Z Has data issue: false hasContentIssue false
  • English
  • Français

Rotational mixing in stellar radiation zones

Published online by Cambridge University Press:  15 November 2004

M. Heydari-Malayeri ,
Ph. Stee ,
J.-P. Zahn  and
J.-P. Zahn
J.-P. Zahn*
Affiliation:
Observatoire de Paris, 92195 Meudon, France
Get access

Abstract

Contrary to what is assumed in building standard stellar models, all stars undergo some mild mixing in their radiation zones. This mixingis due mainly to a slow thermally driven meridional circulation, andshear turbulence presumably contributes to it.It is the rotation of the star which isresponsible for these motions, and therefore the transport of angular momentum must be described in time and space when modeling stellar evolution. This rotational mixing plays an important role in the evolution of massive stars; in particular it determines the late, pre-supernova phases. We review the present state of the problem and discuss briefly the open questions.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 13: Evolution of Massive Stars, Mass Loss and Winds , 2004 , pp. 63 - 79
Copyright
© EAS, EDP Sciences, 2004

Access options

Get access to the full version of this content by using one of the access options below. (Log in options will check for institutional or personal access. Content may require purchase if you do not have access.)