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  Initiation and Early Kinematic Evolution of Solar Eruptions

Cheng, X., Zhang, J., Kliem, B., Török, T., Xing, C., Zhou, Z. J., et al. (2020). Initiation and Early Kinematic Evolution of Solar Eruptions. The Astrophysical Journal, 894(2): 85. doi:10.3847/1538-4357/ab886a.

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Item Permalink: http://hdl.handle.net/21.11116/0000-0006-973A-F Version Permalink: http://hdl.handle.net/21.11116/0000-0006-973B-E
Genre: Journal Article

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Cheng , X.1, Author
Zhang, J., Author
Kliem, B., Author
Török, T., Author
Xing, C., Author
Zhou, Z. J., Author
Inhester, Bernd2, Author              
Ding, M. D., Author
Affiliations:
1Max Planck Institute for Solar System Research, Max Planck Society, Justus-von-Liebig-Weg 3, 37077 Göttingen, DE, ou_1125546              
2Department Sun and Heliosphere, Max Planck Institute for Solar System Research, Max Planck Society, ou_1832289              

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 Abstract: We investigate the initiation and early evolution of 12 solar eruptions, including six active-region hot channel and six quiescent filament eruptions, which were well observed by the Solar Dynamics Observatory, as well as by the Solar Terrestrial Relations Observatory for the latter. The sample includes one failed eruption and 11 coronal mass ejections, with velocities ranging from 493 to 2140 km s−1. A detailed analysis of the eruption kinematics yields the following main results. (1) The early evolution of all events consists of a slow-rise phase followed by a main-acceleration phase, the height–time profiles of which differ markedly and can be best fit, respectively, by a linear and an exponential function. This indicates that different physical processes dominate in these phases, which is at variance with models that involve a single process. (2) The kinematic evolution of the eruptions tends to be synchronized with the flare light curve in both phases. The synchronization is often but not always close. A delayed onset of the impulsive flare phase is found in the majority of the filament eruptions (five out of six). This delay and its trend to be larger for slower eruptions favor ideal MHD instability models. (3) The average decay index at the onset heights of the main acceleration is close to the threshold of the torus instability for both groups of events (although, it is based on a tentative coronal field model for the hot channels), suggesting that this instability initiates and possibly drives the main acceleration.

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Language(s): eng - English
 Dates: 2020
 Publication Status: Published in print
 Pages: -
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 Rev. Method: Peer
 Identifiers: DOI: 10.3847/1538-4357/ab886a
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Title: The Astrophysical Journal
Source Genre: Journal
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Publ. Info: Bristol; Vienna : IOP Publishing; IAEA
Pages: - Volume / Issue: 894 (2) Sequence Number: 85 Start / End Page: - Identifier: ISSN: 0004-637X
CoNE: https://pure.mpg.de/cone/journals/resource/954922828215_3