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Stellar coronal response to differential rotation and flux emergence.

Gibb, G.P.S. and Mackay, D.H. and Jardine, M.M. and Yeates, A.R. (2016) 'Stellar coronal response to differential rotation and flux emergence.', Monthly notices of the Royal Astronomical Society., 456 (4). pp. 3624-3637.

Abstract

We perform a numerical parameter study to determine what effect varying differential rotation and flux emergence has on a star's non-potential coronal magnetic field. In particular we consider the effects on the star's surface magnetic flux, open magnetic flux, mean azimuthal field strength, coronal free magnetic energy, coronal heating and flux rope eruptions. To do this, we apply a magnetic flux transport model to describe the photospheric evolution, and couple this to the non-potential coronal evolution using a magnetofrictional technique. A flux emergence model is applied to add new magnetic flux on to the photosphere and into the corona. The parameters of this flux emergence model are derived from the solar flux emergence profile, however the rate of emergence can be increased to represent higher flux emergence rates than the Sun's. Overall we find that flux emergence has a greater effect on the non-potential coronal properties compared to differential rotation, with all the aforementioned properties increasing with increasing flux emergence rate. Although differential rotation has a lesser effect on the overall coronal properties compared to flux emergence, varying differential rotation does alter the coronal structure. As the differential rotation rate increases, the corona becomes more open, and more non-potential.

Item Type:Article
Keywords:Stars: activity – stars: coronae, Stars: magnetic field, Stars: rotation.
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Status:Peer-reviewed
Publisher Web site:http://dx.doi.org/10.1093/mnras/stv2920
Publisher statement:This article has been accepted for publication in Monthly notices of the Royal Astronomical Society ©: 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
Date accepted:10 December 2015
Date deposited:25 January 2016
Date of first online publication:14 January 2016
Date first made open access:25 January 2016

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