Multi-wavelength Signatures of Magnetic Reconnection of a Flare Associated Coronal Mass Ejection

The evolution of an X2.7 solar flare, that occurred in a complex βγδ magnetic configuration region on 2003 November 3, is discussed utilizing a multiwavelength data set. The Hα images taken from the solar tower telescope at ARIES, Nainital, reveal well-defined footpoint (FP) and loop-top (LT) sources. As the flare evolves, the LT source moves upward and the separation between the two FP sources increases which is consistent with reconnection models of solar flares. The co-alignment of Hα with hard X-ray (HXR) images obtained from RHESSI shows spatial correlation between Hα and HXR footpoints, while the rising LT source in HXR is always located above the LT source seen in Hα. The EUV images of the flaring region at 195 Å taken from SOHO/EIT reveal intense emission from low-lying loops near the active region during the impulsive phase. On the other hand, two bright loops are seen well outside the active region which undergo large scale reorganization during the flare. In radio wavelengths, type III radio bursts are observed few minutes prior to the start of HXR emission at the LT indicating pre-flare coronal activity. Slow drifting type IV bursts, which are observed at lower coronal heights at two time intervals along the flare period, are likely to be associated with the reconnection processes at two different coronal heights. Further, the intense type II radio burst at time inbetween these type IV bursts, but at a relatively larger height indicates the onset of CME and its associated coronal shock wave. The results of this study support the ‘break-out’ scenario observed in multipole magnetic configuration of a flaring region.