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dc.contributor.authorGibb, Gordon Peter Samuel
dc.contributor.authorMackay, Duncan Hendry
dc.contributor.authorJardine, Moira Mary
dc.contributor.authorYeates, A. R.
dc.date.accessioned2016-02-24T13:10:07Z
dc.date.available2016-02-24T13:10:07Z
dc.date.issued2016-03-11
dc.identifier.citationGibb , G P S , Mackay , D H , Jardine , M M & Yeates , A R 2016 , ' Stellar coronal response to differential rotation and flux emergence ' , Monthly Notices of the Royal Astronomical Society , vol. 456 , no. 4 , pp. 3624-3637 . https://doi.org/10.1093/mnras/stv2920en
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 241204702
dc.identifier.otherPURE UUID: 49ddc75d-298e-4e4d-a774-df9a80cbcb51
dc.identifier.otherBibCode: 2016MNRAS.456.3624G
dc.identifier.otherScopus: 84963831850
dc.identifier.otherORCID: /0000-0001-6065-8531/work/58055424
dc.identifier.otherWOS: 000372265800016
dc.identifier.otherORCID: /0000-0002-1466-5236/work/57821818
dc.identifier.urihttp://hdl.handle.net/10023/8298
dc.descriptionGPSG would like to thank the STFC for financial support. DHM would like to thank the STFC and the Leverhulme Trust for financial support. Simulations were carried out on a STFC/SRIF funded UKMHD cluster at St Andrews.en
dc.description.abstractWe 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.
dc.format.extent14
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rights© 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. This work is made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at https://dx.doi.org/10.1093/mnras/stv2920en
dc.subjectStars: activity - stars: coronaeen
dc.subjectStars: magnetic fielden
dc.subjectStars: rotationen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectNDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleStellar coronal response to differential rotation and flux emergenceen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.Applied Mathematicsen
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.1093/mnras/stv2920
dc.description.statusPeer revieweden
dc.identifier.urlhttp://adsabs.harvard.edu/abs/2016MNRAS.456.3624Gen


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