3D Solar Null Point Reconnection MHD Simulations

Details 3D Solar Null Point Reconnection MHD Simulations 3D Solar Null Point Reconnection MHD Simulations

2012-03-05

arxiv.org/abs/1203.1018v1

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

24 pages, 19 figures, submitted to Solar Physics (Springer)

Scientific paper

Numerical MHD simulations of 3D reconnection events in the solar corona have improved enormously over the last few years, not only in resolution, but also in their complexity, enabling more and more realistic modeling. Various ways to obtain the initial magnetic field, different forms of solar atmospheric models as well as diverse driving speeds and patterns have been employed. This study considers differences between simulations with stratified and non-stratified solar atmospheres, addresses the influence of the driving speed on the plasma flow and energetics, and provides quantitative formulae for mapping electric fields and dissipation levels obtained in numerical simulations to the corresponding solar quantities. The simulations start out from a potential magnetic field containing a null-point, obtained from a Solar and Heliospheric Observatory (SOHO) magnetogram extrapolation approximately 8 hours before a C-class flare was observed. The magnetic field is stressed with a boundary motion pattern similar to - although simpler than - horizontal motions observed by SOHO during the period preceding the flare. The general behavior is nearly independent of the driving speed, and is also very similar in stratified and non-stratified models, provided only that the boundary motions are slow enough. The boundary motions cause a build-up of current sheets, mainly in the fan-plane of the magnetic null-point, but does not result in a flare-like energy release. We conclude that the most likely reason for the flare energy release was the additional flux emergence that occurred near the flare site.

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