Global Dynamics of Subsurface Solar Active Regions

Abstract

We present three-dimensional numerical simulations of a magnetic loop evolving in either a convectively stable or unstable rotating shell. The magnetic loop is introduced in the shell in such a way that it is buoyant only in a certain portion in longitude, thus creating an Ω-loop. Due to the action of magnetic buoyancy, the loop rises and develops asymmetries between its leading and following legs, creating emerging bipolar regions whose characteristics are similar to the ones of observed spots at the solar surface. In particular, we self-consistently reproduce the creation of tongues around the spot polarities, which can be strongly affected by convection. We moreover emphasize the presence of ring-shaped magnetic structures around our simulated emerging regions, which we call "magnetic necklace" and which were seen in a number of observations without being reported as of today. We show that those necklaces are markers of vorticity generation at the periphery and below the rising magnetic loop. We also find that the asymmetry between the two legs of the loop is crucially dependent on the initial magnetic field strength. The tilt angle of the emerging regions is also studied in the stable and unstable cases and seems to be affected both by the convective motions and the presence of a differential rotation in the convective cases.

23 pages (ApJ 2-column format), 19 figures, accepted for publication in ApJ

References in corpus (7)

• Global-Scale Turbulent Convection and Magnetic Dynamo Action in the Solar Envelope
• Twisted flux tube emergence from the convection zone to the corona
• Eruption of magnetic flux ropes during flux emergence
• The Counter-kink Rotation of a Non-Hale Active Region
• Flux emergence and coronal eruption
• 3-D non-linear evolution of a magnetic flux tube in a spherical shell: the isentropic case
• How can large-scale twisted magnetic structures naturally emerge from buoyancy instabilities?

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