High-resolution He i 10830 ??Narrowband Imaging for an M-class Flare. II. Multiple Hot Channels: Their Origin and Destination
Wang,Ya1,2; Su,Yingna1,3; Shen,Jinhua4; Yang,Xu5; Cao,Wenda5; Ji,Haisheng1,3
Source PublicationThe Astrophysical Journal
AbstractAbstract In this paper, we report our second-part result for the M1.8 class flare on 2012 July 5, with an emphasis on the initiation process for the flare-associated filament eruption. The data set consists of high-resolution narrowband images in He i 10830 ? and broadband images in TiO 7057 ? taken at Big Bear Solar Observatory with the 1.6 m aperture Goode Solar Telescope. EUV images in different passbands observed by the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory are used to distinguish hot plasma from cool plasma structures during the flare process. High-resolution 10830 ? images clearly show that, below the horizontal fibrils, which correspond to the filament’s spine in full-disk Hα images, a sheared arch filament system (AFS) lies across the penumbra and surrounding satellite sunspots, between which continuous shearing motion is observed. Before the eruption, three microflares occurred successively and were followed by the appearance of three EUV hot channels. Two hot channels erupted, producing two flaring sites and two major peaks in GOES soft X-ray light curves; however, one hot channel’s eruption failed. The 10830 ? imaging enables us to trace the first two hot channels to their very early stage, which is signified by the rising of the AFS after the first two precursors. Continuous flux emergence and localized flare-associated cancellation are observed under the AFS. In addition, EUV ejections were observed during the formation of the EUV hot channels. These observations support the fact that the hot channels are the result of magnetic reconnections during precursors.
KeywordSun: coronal mass ejections (CMEs) Sun: filaments, prominences Sun: flares sunspots
WOS IDIOP:0004-637X-859-2-aac0f7
PublisherThe American Astronomical Society
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Document Type期刊论文
Affiliation1.Key Laboratory for Dark Matter and Space Science, Purple Mountain Observatory, CAS, Nanjing, 210008, People’s Republic of China
2.University of Chinese Academy of Sciences, Beijing, 100049, People’s Republic of China
3.School of Astronomy and Space Science, University of Science and Technology of China, Hefei, Anhui, 230026, People’s Republic of China
4.Xinjiang Astronomical Observatory, CAS, Urumqi, 830011, People’s Republic of China
5.Big Bear Solar Observatory, Big Bear City, CA 92314, USA
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GB/T 7714
Wang,Ya,Su,Yingna,Shen,Jinhua,et al. High-resolution He i 10830 ??Narrowband Imaging for an M-class Flare. II. Multiple Hot Channels: Their Origin and Destination[J]. The Astrophysical Journal,2018,859(2).
APA Wang,Ya,Su,Yingna,Shen,Jinhua,Yang,Xu,Cao,Wenda,&Ji,Haisheng.(2018).High-resolution He i 10830 ??Narrowband Imaging for an M-class Flare. II. Multiple Hot Channels: Their Origin and Destination.The Astrophysical Journal,859(2).
MLA Wang,Ya,et al."High-resolution He i 10830 ??Narrowband Imaging for an M-class Flare. II. Multiple Hot Channels: Their Origin and Destination".The Astrophysical Journal 859.2(2018).
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