[P-EM14] Frontiers in solar physics

[PEM14-09] Long-term Data-driven MHD Simulation of Solar Active Region 11283

*Yeongmin Kang¹, Takafumi Kaneko¹, Kanya Kusano¹ (1.Institute for Space-Earth Environmental Research)

Keywords:Sun, Solar flare

Various explosive events occur in the Sun. Solar flares, one of the explosive events, are caused by the release of magnetic energy stored in the coronal magnetic field and sometimes accompanied by coronal mass ejections (CMEs) that eject energetic particles into interplanetary space. Solar flares occur in solar active regions (ARs), usually known as sunspots, where strong magnetic fields are present on the photosphere. The coronal magnetic field above the active region is known to be the source of the flares. It is also known that magnetic reconnections and MHD instabilities are important process in the flare production. Therefore, information on the three-dimensional coronal magnetic field is necessary to study solar flares. However, the physical mechanism of solar flares is still not clearly understood because it is hard to observe the coronal magnetic field directly. That is, understanding the physical mechanism of solar flares has become one of the most important issues in solar physics. For this reason, various methods have been developed to calculate and analyze the three-dimensional coronal magnetic field using the currently observable two-dimensional photospheric magnetic field. In this study, we conducted a data-driven magnetohydrodynamic (MHD) simulation to investigate the relationship between magnetic field evolutions in the solar active region 11283 (AR 11283) and the occurrence of M5.3 class flare. The simulation method is basically based on the data-driven method introduced by Kaneko et al. (2021). This method uses time-series photospheric magnetic field data (SDO/HMI) as input data (bottom boundary condition) and can calculate the temporal evolution of the coronal magnetic field. Since the time-series observational magnetic field data are used, it is expected to reproduce a more realistic coronal magnetic field. The simulation period was from 2011 September 4, 19:48 UT to 2011 September 6, 06:48 UT including the M5.3 class flare event (2011 September 6, 01:59 UT), and the time interval of the input data was 1 hour. As a result, the growth of the MHD instability was reproduced, and the increasing rate of the kinetic energy changed with this growth. Furthermore, the peak time of the real M5.3 class flare and the peak time of the kinetic energy of the plasma in the simulation almost coincided. In addition, the distribution of the flare ribbons observed in SDO/AIA 1600 Å matches the footpoints of high magnetic twist field lines in our simulation.