The Study of Flare and Relative CME within the Solar Active Region 10537 on Jan.8^th,2004

By means of the Hα、UV、EUV、WL、17GHz and photospheric line-of-sight magnetic field observations, we have studied a M1.3 flare in AR10537 with δ configuration on January 8, 2004. The flare consisted of two main flare ribbons locating on regions of opposite magnetic polarities and covering the partial penumbra of the AR's sunspots. However, a remote flaring ribbon can be clearly seen from these images of Hα、1700Å and 195Å in its south, which was closely associated with the partial disappearance of a large Hα filament in its east. Then EIT dimming was formed in this remote brightening. These observations suggest a rearrangement of large-scale coronal structure and a reduction of the density near the footpoint of the remote flare brightenings as a result of chromosphere evaporation involved in the flare. The flare showed good temporal and spatial relationships with a quick partial halo CME(coronal mass Ejections) observed by SOHO/LASCO, and it is very likely that they are two different manifestations of the same magnetic eruption process in the corona. Therefore, we identify that the flare and the associated coronal dimmings are just the on-disk source region of the CME on solar disk.