Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmsh52a..06k&link_type=abstract
American Geophysical Union, Fall Meeting 2008, abstract #SH52A-06
Astronomy and Astrophysics
Astrophysics
7500 Solar Physics, Astrophysics, And Astronomy, 7509 Corona, 7513 Coronal Mass Ejections (2101), 7519 Flares, 7526 Magnetic Reconnection (2723, 7835)
Scientific paper
Solar eruptions, which arise as flares and coronal mass ejection (CME), are the most energetic phenomena in our solar system, and can often influence even the geo-space environment. However, the initiation mechanism and the physical condition for the onset of them are not yet well understood. The objective of this study is to clarify how the multiscale interaction between small scale magnetic reconnection and the large scale evolution of the solar coronal magnetic field interact with each other for the initiation of solar eruptions. In order to obtain that, we have developed a realistic magnetohydrodynamics (MHD) simulation, which is driven by a high resolution vector magnetogram observed by Solar Optical Telescope (SOT) onboard Hinode. The simulation is performed by incorporating the advanced magnetofrictional model for the nonlinear force-free extrapolation and the three different MHD models for active region, global corona, and the interplanetary space, respectively. Using the model, we have successfully performed the first-ever data- driven simulation of the eruptive event caused by the X-class solar flare, which occurred in the active region NOAA 10930 on Dec. 13, 2006. The simulation result indicates that magnetic reconnection triggered in a strongly sheared region causes a large scale eruption, in which a plasmoid with helical magnetic flux is ejected at super-Alfvenic speed. The direction and speed of plasmoid ejection are well consistent with the observation by EUV imaging spectrometer (EIS) onboard Hinode. The evolution of field line topology is also consistent with the SOT observation of flare ribbons. The propagation of CME, which is formed as a result of the plasmoid ejection, is calculated by handing over the output data of the active region model to the coronal model. The results indicate that the tether cutting scenario is well consistent with the observation, and also suggest us that the data-driven simulation might be usable for some kind of now-casting simulation of solar eruption, which could assess what type of solar eruption is able to arise from particular active regions.
Asano Eiji
Inoue Susumu
Kataoka Ryuho
Kusano Kanya
Matsumoto Toshio
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