Multi-wavelength Observation of Initiation Phase of Filament Eruption
Monday, 15 December 2014
We have examined a nonthermal emission of a preflare activity associated with M-class flare. This activity resulted in a filament eruption that was developed into a halo CME. It was observed by microwave from Nobeyama Radioheliograph (NoRH) at 17 GHz and 34 GHz, Hard X-ray from Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) at 6-80 keV, and EUV from Atmospheric Imaging Assembly (AIA) onboard Solar Dynamics Observatory (SDO). We found that a microwave nonthermal source appeared near a southern footpoint of the filament system during the preflare phase. Then it moved systematically away from there in the direction parallel to two-ribbons together with the rapid eruption of the filament system. It implies that the particle acceleration of the flare started near the southern footpoint of the filament system and, thus, it provided a decisive factor for the eruption of it. During the preflare phase, Hard X-ray source also appeared in the position close to microwave source and their source positions lined up depending on their energy-bands. Unfortunately, there is no RHESSI data during the main flare because it passed night-part of the earth. Here, we present the detail investigation of physical parameters and emission mechanism of the preflare nonthermal emission based on the imaging spectroscopy of microwave and Hard X-ray.