Astronomy and Astrophysics – Astrophysics – Solar and Stellar Astrophysics
Scientific paper
2010-08-28
2010, ApJ, 723, 229
Astronomy and Astrophysics
Astrophysics
Solar and Stellar Astrophysics
ApJ, accepted on 08/27/2010
Scientific paper
10.1088/0004-637X/723/1/229
The pre-CME structure is of great importance to understanding the origin of CMEs, which, however, has been largely unknown for CMEs originating from active regions. In this paper, selected for studying are 16 active-region coronal arcades whose gradual inflation lead up to CMEs. 12 of them clearly build upon post-eruptive arcades resulting from a preceding eruption. The observed inflation sustains for 8.7 +/- 4.1 h, with the arcade rising from 1.15 +/- 0.06 Rsun to 1.36 +/- 0.07 Rsun within the EIT field of view (FOV). The rising speed is less than 5 km s-1 for most of the time. Only at the end of this quasi-static stage, it increases to tens of kilometers per second over tens of minutes. The arcade then erupts out of the EIT FOV as a CME with similar morphology. This pre-CME structure is apparently unaffected by the flares occurring during its quasi-static inflation phase, but is closely coupled with the flare occurring during its acceleration phase. For four events that were observed on the disk, it is found that the gradual inflation of the arcade is accompanied by significant helicity injection from photosphere. In particular, a swirling structure, which is reminiscent of a magnetic flux rope, was observed in one of the arcades over 4 h prior to the subsequent CME, and the growth of the arcade is associated with the injection of helicity of opposite sense into the active region via flux emergence. We propose a four-phase evolution paradigm for the observed CMEs, i.e., a quasi-static inflation phase which corresponds to the buildup of magnetic free energy in the corona, followed by the frequently observed three-phase paradigm, including an initial phase, an acceleration phase and a gradual phase.
Liu Chang
Liu Rui
Park Sung-Hong
Wang Haimin
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