Coronal heating and nanoflares : current sheet formation and heating
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Aims: Solar photospheric footpoint motions can produce strong, localised currents in the corona. A detailed understanding of the formation process and the resulting heating is important in modelling nanoflares, as a mechanism for heating the solar corona. Methods: A 3D MHD simulation is described in which an initially straight magnetic field is sheared in two directions. Grid resolutions up to 5123 were used and two boundary drivers were considered; one where the boundaries are continuously driven and one where the driving is switched off once a current layer is formed. Results: For both drivers a twisted current layer is formed. After a long time we see that, when the boundary driving has been switched off, the system relaxes towards a lower energy equilibrium. For the driver which continuously shears the magnetic field we see a repeating cycle of strong current structures forming, fragmenting and decreasing in magnitude and then building up again. Realistic coronal temperatures are obtained.
Bowness , R , Hood , A W & Parnell , C E 2013 , ' Coronal heating and nanoflares : current sheet formation and heating ' , Astronomy & Astrophysics , vol. 560 , A89 . https://doi.org/10.1051/0004-6361/201116652
Astronomy & Astrophysics
© 2013, ESO. A&A 560, A89 (2013). Reproduced with permission from the publishers.
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