Hostname: page-component-7dd5485656-wxk4p Total loading time: 0 Render date: 2025-10-31T17:14:30.591Z Has data issue: false hasContentIssue false
  • English
  • Français

Magnetorotational instability in Ap star envelopes

Published online by Cambridge University Press:  02 March 2005

Reiner Arlt
Reiner Arlt
Affiliation:
Astrophysikalisches Institut Potsdam, An der Sternwarte 16, D-14482 Potsdam, Germany email: rarlt@aip.de
Rights & Permissions [Opens in a new window]

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.

The rotational evolution of the radiative zone of magnetic Ap stars is investigated with numerical simulations. An angular-velocity profile decreasing with axis distance in combination with a magnetic field leads to a magnetorotational instability. The resulting flows efficiently transport angular momentum outwards. The corresponding decay of angular-velocity gradients in the radiative zone is estimated to take about 10–100 million years.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Keywords

MHDinstabilitiesstars: rotation

Information

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2004 , Issue IAUS224 , July 2004 , pp. 103 - 108
Copyright
© 2004 International Astronomical Union