Transition-region explosive events produced by plasmoid instability
arXiv:1811.01559 · doi:10.1088/1674-4527/19/5/67
Abstract
Magnetic reconnection is thought to be a key process in most of solar eruptions. Thanks to high-resolution observations and simulations, the studied scale of reconnection process has become smaller and smaller. Spectroscopic observations show that the reconnection site can be very small, which always exhibits a bright core and two extended wings with fast speeds, i.e., transition-region explosive events. In this paper, using the PLUTO code, we perform a 2-D magnetohydrodynamic simulation to investigate the small-scale reconnection in double current sheets. Based on our simulation results, such as the line-of-sight velocity, number density and plasma temperature, we can synthesize the line profile of Si IV 1402.77 A which is a well known emission line to study the transition-region explosive events on the Sun. The synthetic line profile of Si IV 1402.77 A is complex with a bright core and two broad wings which can extend to be nearly 200 km/s. Our simulation results suggest that the transition-region explosive events on the Sun are produced by plasmoid instability during the small-scale magnetic reconnection.
15 pages, 5 figures, 1 table, accepted by RAA
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- Flaring-associated Complex Dynamics in Two M-dwarfs Revealed by Fast, Time-resolved Spectroscopy
- Simultaneous Observations of Chromospheric Evaporation and Condensation during a C-class Flare
- Moving structures in ultraviolet bright points: observations from Solar Orbiter/EUI
- An investigation of flare emissions at multiple wavelengths
- The Ellerman bomb and Ultraviolet burst triggered successively by an emerging magnetic flux rope