H Dimmings Associated with the X1.6 Flare and Halo Coronal Mass Ejection on 2001 October 19

Abstract

As the optical counterpart of coronal dimmings, we present the first direct evidence of Halpha associated with the X1.6 flare, filament eruption, and coronal mass ejection (CME) that occurred on 2001 October 19. As two main Halpha flare ribbons parallel to the erupting filament slowly separated, two other ribbons first quickly expanded near the feet of the filament, then their interiors substantially dimmed and became darker than the preflare brightness. This formed two dimming regions with sharp bright edges. The two Halpha were different from the flare nimbus and the Halpha darkenings found by Ellison, McKenna, & Reid and Neidig et al., respectively, but similar to the coronal double dimmings studied by Sterling & Hudson. The coronal of the event were also observed in 171 Angstrom images from the Transition Region and Coronal Explorer (TRACE). The 171 Angstrom and Halpha showed very similar evolutions and occurred at the same two sites with opposite magnetic polarities. They formed in the course of the filament eruption, and after the eruption, some 171 Angstrom loops of the postflare arcade developed to connect their inner edges while some loops with footpoints near their outer edges disappeared. Observations from the Solar and Heliospheric Observatory Extreme-ultraviolet Imaging Telescope (SOHO/EIT) showed more extended associated with the eruption. Only a small portion of EIT was cospatial with the Halpha dimmings, while the major other portion was associated with the disappeared 171 Angstrom loops. These joint observations are interpreted by using the flux rope model of CMEs, in which the Halpha represent the evacuated feet of the erupted flux rope. The mass supply of the halo CME could be coming from both the erupted flux rope itself and the lost material close to the flare footpoint regions as shown by Halpha dimmings.