Abstract

Contributed Talk - Splinter Solar

Wednesday, 23 September 2020, 14:52   (virtual room L)

A data-driven magnetohydrodynamic simulation of a successful solar eruption

Ze Zhong, Yang Guo, Thomas Wiegelmann, Mingde Ding
Nanjing University; Max Planck Institute for Solar System Research

Solar eruptions are driven by instabilities of magnetic flux ropes. They can be either successful erupt and propagating into the interplanetary space, or remain confined in the corona. The eruption mechanisms are still an active area of research. One mechanism is based on ideal magnetohydrodynamic instabilities. We can simulate such eruptions by using the measured solar photospheric magnetic field vector as boundary condition. Here we report a magnetohydrodynamic modeling for the 04 August 2011 eruption and successfully reproduce an observed solar flare associated with a coronal mass ejection. The morphology of the flare ribbons and kinematics of the flux rope revealed by the simulation agree with the observations. The flux rope undergoes a two acceleration phases, a linear slow rise phase followed by a fast acceleration phase. We use stereoscopic observations by two instruments to reconstruct the eruption path and measure the height time profile of the acceleration. It is found that the profile of the latter phase is approximately matched by the acceleration profile under the assumption of a simplified current ring model. We suggest that a torus instability is the key to drive this flare fast acceleration.