Multi-wavelength Observation of Filament Eruption associated with M-class Flare

We have investigated a M-class flare associated with filament eruption which developed into a Halo CME. The M-class flare occurred in 2011 August 4. For this study, we used the Nobryama Radioheliograph (NoRH) 17 and 34 GHz, RHESSI Hard X-ray satellite, and Atmo- spheric Imaging Assembly (AIA) and the Heliospheric Magentic Imager(HMI) onboard the Solar Dynamic Observatory (SDO). During the pre-eruption phase, clear nonthermal emission was detected in microwaves of NoRH and hard-X-ray of RHESSI. At the moment that the nonthermal emission start, the nonthermal sources appeared at the one edge of the filament structure on a polarity inversion line, and the slowing rising filament structure in AIA 94A underwent a sudden acceleration on its ascendance. Magnetograms showed converging motion of magnetic elements at the source position of HXR and MW. Based on the results, we conjecture that the plausible trigger of the filament eruption is magnetic reconnections at the HXR source position by converging motion of magnetic elements. In addition, we will discuss on the magnetic flux variation before and after the eruption based on the result of Nonlinear force-free field model.