TY - JOUR
T1 - A Data-constrained Magnetohydrodynamic Simulation of the X1.0 Solar Flare of 2021 October 28
AU - Yamasaki, Daiki
AU - Inoue, Satoshi
AU - Bamba, Yumi
AU - Lee, Jeongwoo
AU - Wang, Haimin
N1 - Funding Information:
SDO is a mission of NASA's Living With a Star Program. This work utilizes data from the National Solar Observatory Integrated Synoptic Program, which is operated by the Association of Universities for Research in Astronomy, under a cooperative agreement with the National Science Foundation and with additional financial support from the National Oceanic and Atmospheric Administration, the National Aeronautics and Space Administration, and the United States Air Force. The GONG network of instruments is hosted by the Big Bear Solar Observatory, High Altitude Observatory, Learmonth Solar Observatory, Udaipur Solar Observatory, Instituto de Astrofísica de Canarias, and Cerro Tololo Interamerican Observatory. This work was supported by MEXT/JSPS KAKENHI grant No. JP21J14036 and 21K20379. This work was also supported by JSPS Overseas Challenge Program for Young Researchers. This study is partially supported by National Science Foundation AGS-2145253, AGS-1954737, and AST-2204384. J.L. acknowledges support by NASA grants, 80NSSC18K1705 and 80NSSC21K1671. Visualization of magnetic field lines are produced by VAPOR ( www.vapor.ucar.edu ), a product of the Computational Information Systems Laboratory at the National Center for Atmospheric Research (Li et al. ).
Funding Information:
SDO is a mission of NASA's Living With a Star Program. This work utilizes data from the National Solar Observatory Integrated Synoptic Program, which is operated by the Association of Universities for Research in Astronomy, under a cooperative agreement with the National Science Foundation and with additional financial support from the National Oceanic and Atmospheric Administration, the National Aeronautics and Space Administration, and the United States Air Force. The GONG network of instruments is hosted by the Big Bear Solar Observatory, High Altitude Observatory, Learmonth Solar Observatory, Udaipur Solar Observatory, Instituto de Astrofísica de Canarias, and Cerro Tololo Interamerican Observatory. This work was supported by MEXT/JSPS KAKENHI grant No. JP21J14036 and 21K20379. This work was also supported by JSPS Overseas Challenge Program for Young Researchers. This study is partially supported by National Science Foundation AGS-2145253, AGS-1954737, and AST-2204384. J.L. acknowledges support by NASA grants, 80NSSC18K1705 and 80NSSC21K1671. Visualization of magnetic field lines are produced by VAPOR (www.vapor.ucar.edu), a product of the Computational Information Systems Laboratory at the National Center for Atmospheric Research (Li et al. 2019).
Publisher Copyright:
© 2022. The Author(s). Published by the American Astronomical Society.
PY - 2022/12/1
Y1 - 2022/12/1
N2 - The solar active region NOAA 12887 produced a strong X1.0 flare on 2021 October 28, which exhibits X-shaped flare ribbons and a circle-shaped erupting filament. To understand the eruption process with these characteristics, we conducted a data-constrained magnetohydrodynamics simulation using a nonlinear force-free field of the active region about an hour before the flare as the initial condition. Our simulation reproduces the filament eruption observed in the Hα images of GONG and the 304 Å images of SDO/AIA, and suggests that two mechanisms can possibly contribute to the magnetic eruption. One is the torus instability of the preexisting magnetic flux rope (MFR) and the other is upward pushing by magnetic loops newly formed below the MFR via continuous magnetic reconnection between two sheared magnetic arcades. The presence of this reconnection is evidenced by the SDO/AIA observations of the 1600 Å brightening in the footpoints of the sheared arcades at the flare onset. To clarify which process is more essential for the eruption, we performed an experimental simulation in which the reconnection between the sheared field lines is suppressed. In this case too, the MFR could erupt, but at a much reduced rising speed. We interpret this result as indicating that the eruption is not only driven by the torus instability, but additionally accelerated by newly formed and rising magnetic loops under continuous reconnection.
AB - The solar active region NOAA 12887 produced a strong X1.0 flare on 2021 October 28, which exhibits X-shaped flare ribbons and a circle-shaped erupting filament. To understand the eruption process with these characteristics, we conducted a data-constrained magnetohydrodynamics simulation using a nonlinear force-free field of the active region about an hour before the flare as the initial condition. Our simulation reproduces the filament eruption observed in the Hα images of GONG and the 304 Å images of SDO/AIA, and suggests that two mechanisms can possibly contribute to the magnetic eruption. One is the torus instability of the preexisting magnetic flux rope (MFR) and the other is upward pushing by magnetic loops newly formed below the MFR via continuous magnetic reconnection between two sheared magnetic arcades. The presence of this reconnection is evidenced by the SDO/AIA observations of the 1600 Å brightening in the footpoints of the sheared arcades at the flare onset. To clarify which process is more essential for the eruption, we performed an experimental simulation in which the reconnection between the sheared field lines is suppressed. In this case too, the MFR could erupt, but at a much reduced rising speed. We interpret this result as indicating that the eruption is not only driven by the torus instability, but additionally accelerated by newly formed and rising magnetic loops under continuous reconnection.
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U2 - 10.3847/1538-4357/ac9df4
DO - 10.3847/1538-4357/ac9df4
M3 - Article
AN - SCOPUS:85143733224
SN - 0004-637X
VL - 940
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 2
M1 - 119
ER -