An MHD Model of the Major Solar Flare on 2006 December 13

Details An MHD Model of the Major Solar Flare on 2006 December 13 An MHD Model of the Major Solar Flare on 2006 December 13

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsh42a..10k&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SH42A-10

Astronomy and Astrophysics

Astrophysics

[7519] Solar Physics, Astrophysics, And Astronomy / Flares, [7524] Solar Physics, Astrophysics, And Astronomy / Magnetic Fields, [7526] Solar Physics, Astrophysics, And Astronomy / Magnetic Reconnection, [7959] Space Weather / Models

Scientific paper

Solar storm caused by major solar flare is the source of heliospheric and geo-magnetospheric disturbance. However, the onset mechanism of flare is not well understood yet. Aiming at revealing the initiation mechanism of solar storm, we have recently developed a new realistic magnetohydrodynamic (MHD) model of the major solar flare on 2006 December 13, based on the observation by Solar Optical Telescope (SOT) onboard Hinode solar physics satellite. We first calculated the nonlinear force-free field (NLFFF) of active region NOAA 10930 using the vector magnetogram observed by Hinode/SOT. Second, we carried out the three-dimensional MHD simulation by imposing photospheric variation which corresponds to the magnetic flux emerging activity seen prior to the onset of the flare. As a result, we have successfully simulated a solar eruption, in which magnetic reconnection drives super Alfvenic plasma jet from the flaring site. The comparative analysis with the spectroscopic observation by an EUV imaging spectrometer (EIS) on Hinode indicates that both the structure and the speed of jet in the numerical simulation are well consistent with the observation. The results encourage us that the MHD model driven by the magnetogram observation is able to be a powerful tool to understand the initiation process of solar flare.

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