Numerical simulations of rotating sunspots

Gert Botha, Alistair Rucklidge, F. H. Busse, Neal Hurlburt

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Abstract

A numerical model of idealized, axisymmetric, rotating sunspots is presented. The model contains a compressible plasma described by the nonlinear MHD equations, with density and temperature gradients simulating the upper layer of the sun’s convection zone. The solution forms a central flux tube in the cylindrical numerical domain, with convection cells pushing the magnetic field to the axis. When the numerical domain is rotated with a constant angular velocity, the umbra rotates as a rigid body while the surrounding convection cells show a swirling, vortical flow. As a result, the azimuthal velocity and magnetic field have their maximum values close to the flux tube, inside the innermost convection cell.
Original languageEnglish
Title of host publicationProceedings of SOHO-17 ‘10 Years of SOHO and Beyond’
EditorsH. Lacoste
Place of PublicationNoordwijk, The Netherlands
PublisherESA Publications Division, ESTEC
Number of pages4
Volume617
ISBN (Print)978-9290929284
Publication statusPublished - Jul 2006

Publication series

NameESA SP
PublisherESA Publications Division, ESTEC

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