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Destruction of Be star disk by large scale magnetic fields

Published online by Cambridge University Press:  28 July 2017

Asif ud-Doula Open the ORCID record for Asif ud-Doula [Opens in a new window] ,
Stanley Owocki ,
Nathaniel (Dylan) Kee  and
Michael Vanyo
Asif ud-Doula
Affiliation:
Penn State Worthington Scranton, Dunmore, PA, USA, email: [email protected]
Stanley Owocki
Affiliation:
University of Delaware, Newark, DE, USA
Nathaniel (Dylan) Kee
Affiliation:
University of Tubingen, Tubingen, Germany
Michael Vanyo
Affiliation:
Penn State Worthington Scranton, Dunmore, PA, USA, email: [email protected]
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Abstract

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Classical Be stars are rapidly rotating stars with circumstellar disks that come and go on time scale of years. Recent observational data strongly suggests that these stars lack the 10% incidence of global magnetic fields observed in other main-sequence B stars. Such an apparent lack of magnetic fields may indicate that Be disks are fundamentally incompatible with a significant large scale magnetic field. In this work, using numerical magnetohydrodynamics (MHD) simulations, we show that a dipole field of only 100G can lead to the quick disruption of a Be disk. Such a limit is in line with the observational upper limits for these objects.

Keywords

stars: emission-lineBestars: magnetic fieldsstars: mass loss(magnetohydrodynamics:) MHD
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S329: The Lives and Death-Throes of Massive Stars , November 2016 , pp. 453
Copyright
Copyright © International Astronomical Union 2017