Magnetohydrostatic modelling of stellar coronae
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We introduce to the stellar physics community a method of modelling stellar coronae that can be considered to be an extension of the potential field. In this approach, the magnetic field is coupled to the background atmosphere. The model is magnetohydrostatic and is a balance between the Lorentz force, the pressure gradient and gravity. Analytical solutions are possible and we consider a particular class of equilibria in this paper. The model contains two free parameters and the effects of these on both the geometry and topology of the coronal magnetic field are investigated. A demonstration of the approach is given using a magnetogram derived from Zeeman–Doppler imaging of the 0.75 M⊙ M-dwarf star GJ 182.
MacTaggart , D , Gregory , S , Neukirch , T & Donati , J-F 2016 , ' Magnetohydrostatic modelling of stellar coronae ' Monthly Notices of the Royal Astronomical Society , vol 456 , no. 1 , pp. 767-774 . DOI: 10.1093/mnras/stv2714
Monthly Notices of the Royal Astronomical Society
© 2016, Publisher / the Author(s). This work is made available online in accordance with the publisher’s policies. This is the author created, accepted version manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at mnras.oxfordjournals.org / https://dx.doi.org/10.1093/mnras/stv2714
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