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New evidence for the reconnection of sliding magnetic field observed by the NVST telescope at the Yunnan Observatory
[ Instrument Network Instrument Development ] Recently, the Shenyuan Light and other people of the Chinese Academy of Sciences, Yunnan Observatory, used the high-resolution observation data of the New Vacuum Solar Telescope (NVST) to report the fan-spine for the first time. The phenomenon of the back and forth sliding motion of the circular flare band under the magnetic field configuration, and indicates that the motion reflects the fine physical process of the three-dimensional magnetic field reconnection in the quasi-demarcation layer of the sector. The International Journal of Astronomy, The Astrophysical Journal Letters, published their latest research on October 29.
Magnetic field reconnection, also known as magnetic field quenching, is a very important fast energy release process in astrophysics. It converts magnetic free energy into particle kinetic energy, thermal energy and radiant energy through the disconnection and reconnection of magnetic lines of force. Magnetic reconnection plays a central role in solar burst activity, but the understanding of its detailed physical processes has not been clear for many years. Because the flare band is usually formed by high-energy particles accelerated by magnetic field reconnection along the magnetic field lines to bombard the low-level atmospheric plasma, researchers usually observe the evolution of the flare band and then observe the occurrence and development of magnetic field reconnection. For example, the conjugated double-band flares commonly seen in flares show the phase and reverse motions of the magnetic field reconnection position, respectively.
The sector-ridge magnetic field system is a special structure that is common in the corona and contains a three-feed magnetic zero. It usually occurs in the presence of a counter-polar magnetic field in a magnetic field of a certain polarity. The outburst-ridge magnetic system outbreak usually results in three flare speeds, the central flare band associated with the inner ridge magnetic field lines, the circular flare speed associated with the fan flux line around the central flare band, and the far region associated with the outer ridge magnetic field lines. Flare belt.
Shen Yuan Deng et al. used the nonlinear forceless field push method to obtain the three-dimensional coronal magnetic field and revealed the sector-ridge magnetic field structure related to the explosion, which confirmed the relationship between each flare band and each magnetic line. The high-speed back and forth motion of the circular flare band was observed for the first time. According to the analysis results, they believe that the back and forth motion of the flare band is caused by the high energy particles accelerated by the recombination of the sliding magnetic field occurring in the sector magnetic boundary layer. The flare zone first moves northward. This is because the dark strip below the fan surface erupts from south to north under the action of magnetic cancellation, so that the magnetic boundary of the magnetic boundary layer of the squeezed fan occurs from south to north, and the flare band follows. The southward movement may be the result of the magnetic reconnection position in the sector magnetic boundary layer moving from north to south during the recovery or oscillation of the system due to the weakening or stopping of the dark strip.
The research results were supported by the National Natural Science Foundation's Outstanding Youth Science Fund, key projects, face-to-face projects, the Yunnan Basic Research Program, the Yunnan Provincial Ten Thousand Plan Youth Talents, and the Western Lights Young Scholars Program of the Chinese Academy of Sciences.