Hostname: page-component-8448b6f56d-tj2md Total loading time: 0 Render date: 2024-04-24T08:32:32.930Z Has data issue: false hasContentIssue false
  • English
  • Français

The Rise of a Magnetic Flux Tube through the Radiative Envelope of a 9 M⊙ Star

Published online by Cambridge University Press:  12 April 2016

J. P. Cassinelli  and
K. B. MacGrego
J. P. Cassinelli
Affiliation:
NCAR, High Altitude Observatory, Boulder, CO 80307-3000 Astronomy Department, University of Wisconsin, Madison, WI 53706-1582
K. B. MacGrego
Affiliation:
NCAR, High Altitude Observatory, Boulder, CO 80307-3000

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.

We explore the possibility that the magnetic field generated by a dynamo at the interface between the convective core and radiative envelope of a massive star can be transported to the surface by buoyancy.

Type
4. Aperiodic Variations
Information
International Astronomical Union Colloquium , Volume 175: The Be Phenomenon in Early-Type Stars , 2000 , pp. 337 - 343
Copyright
Copyright © Astronomical Society of the Pacific 2000

References

Parker, E.N. 1993, ApJ 408, 707 CrossRefGoogle Scholar
MacGregor, K.B., Charbonneau, P. 1997, ApJ 486, 484 CrossRefGoogle Scholar
Charbonneau, P., MacGregor, K.B. 1997, ApJ 486, 502 Google Scholar
Maheswaran, M., Cassinelli, J.P. 1988, ApJ 335, 931 CrossRefGoogle Scholar
Maheswaran, M., Cassinelli, J.P. 1992, ApJ 386, 695 Google Scholar