Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh53c..04k&link_type=abstract
American Geophysical Union, Fall Meeting 2011, abstract #SH53C-04
Astronomy and Astrophysics
Astrophysics
[7513] Solar Physics, Astrophysics, And Astronomy / Coronal Mass Ejections, [7519] Solar Physics, Astrophysics, And Astronomy / Flares, [7526] Solar Physics, Astrophysics, And Astronomy / Magnetic Reconnection
Scientific paper
Solar eruptions, which are observed as flares and/or coronal mass ejections (CMEs), are catastrophic phenomena biggest in our solar system. However, the physical condition for the onset of them is not yet well understood. In this paper, we have performed a systematic computer simulation aiming to understand the role of flux emergence as the trigger of solar eruptions. We adopt the sheared magnetic arcade, which is given by the linear force-free field, as the initial condition, and inject magnetic fluxes, which have various structures, from below the solar surface into the arcade. As results of them, we have obtained the following findings. First, flux emergence into the sheared magnetic arcade can trigger a large scale eruption which well correspond to the onset of flare and/or the launching of CMEs, if and only if the emerged magnetic field is directed to two different azimuths within some width of angle. Second, we found that the emerged magnetic fields of the two different azimuths cause the extended flare reconnection, which may drive two-ribbon flare, in different manners from each other. In the first case, twisted flux tube is formed by the reconnection between the pre-existing field and the emerged field, and it erupts upward due to the loss of equilibrium, resulting in the flare reconnection. In the second case, however, the arcade first collapses into the center due to the reconnection between the arcade and the emerged flux before any flux tube is formed. The collapse of arcade results in the flare reconnection, which creates the flux tube above the reconnection region. Although the magnetic structure of the both cases, respectively called "erupt-to-collapse" and "collapse-to-erupt," well correspond to the CSHKP standard morphology of solar flare, the onset processes of them should be explained as the consequence of different causality. The dependency of the two processes on the initial magnetic shear and the amount of injected flux are also investigated. Finally, we discuss on the applicability of the simulation results to explain the observation, based on the comparison of simulation with the observations by Solar Optical Telescope onboard Hinode satellite.
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