Large-scale Activities in the 2003 October 29 Flare

We present a multiwavelength study of the 2003 October 29 X10 Flare using the data from Improved Solar Observing Optical Network (ISOON), the Solar and Heliospheric Observatory (SOHO), Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI), Transition Region and Coronal Explorer (TRACE), and Owens Valley Solar Array (OVSA). Our study is focused on the large-scale, post-eruption activity on the Sun associated with CMEs, whereas other existing studies are concentrated on the flare core region. In specific, we found two extended remote brightenings and coronal dimmings observed at H-alpha (ISOON) and at extreme ultraviolet (SOHO/EIT) wavelengths, respectively, which are more than 3× 105 km away from the main flare site. These remote H-alpha brightenings are located on the edge of coronal holes that showed dimming after the flare. We consider it unlikely that the remote brightenings are produced by Moreton waves, because they are almost simultaneous with the main flare emissions observed at hard X-ray and microwave wavelengths. We suggest that they rather represent heating of the chromosphere by the flare-accelerated electrons traveling along the large-scale magnetic loops connecting the flare core to the remote patches. We examine the relationship between the HXR footpoint motions in the flare core and the dynamics of the remote patches in order to explore the large-scale magnetic reconfiguration that is responsible for the flare and CME.