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Fine Structures and Overlying Loops of Confined Solar Flares View all abstracts by submitter

Shuhong Yang   Submitted: 2014-09-01 18:38

Using the Hα observations from the New Vacuum Solar Telescope at Fuxian Solar Observatory, we focus on the fine structures of three confined flares and the issue why all the three flares are confined instead of eruptive. All the three confined flares take place successively at the same location and have similar morphologies, so can be termed homologous confined flares. In the simultaneous images obtained by the Solar Dynamics Observatory, many large-scale coronal loops above the confined flares are clearly observed in multi-wavelengths. At the pre-flare stage, two dipoles emerge near the negative sunspot, and the dipolar patches are connected by small loops appearing as arch-shaped Hα fibrils. There exists a reconnection between the small loops, and thus the Hα fibrils change their configuration. The reconnection also occurs between a set of emerging Hα fibrils and a set of pre-existing large loops, which are rooted in the negative sunspot, a nearby positive patch, and some remote positive faculae, forming a typical three-legged structure. During the flare processes, the overlying loops, some of which are tracked by activated dark materials, do not break out. These direct observations may illustrate the physical mechanism of confined flares, i.e., magnetic reconnection between the emerging loops and the pre-existing loops triggers flares and the overlying loops prevent the flares from being eruptive.

Authors: Shuhong Yang, Jun Zhang, and Yongyuan Xiang
Projects: GOES X-rays ,Other,SDO-AIA,SDO-HMI

Publication Status: Accepted for publication in ApJL.
Last Modified: 2014-09-03 13:12
Go to main E-Print page  A Challenging Solar Eruptive Event of 18 November 2003 and the Causes of the 20 November Geomagnetic Superstorm. IV. Unusual Magnetic Cloud and Overall Scenario  THE IMPACT OF A FILAMENT ERUPTION ON NEARBY HIGH-LYING COOL LOOPS  Edit Entry  Download Preprint  Delete Entry 

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