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High-resolution He I 10830 angstrom 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
2018-06-01
Source PublicationASTROPHYSICAL JOURNAL
ISSN0004-637X
Volume859Issue:2Pages:11
Abstract

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 110830 angstrom and broadband images in TiO 7057 angstrom 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 angstrom images clearly show that, below the horizontal fibrils, which correspond to the filament's spine in full-disk Ha 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 angstrom 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
DOI10.3847/1538-4357/aac0f7
WOS KeywordCORONAL MASS EJECTIONS ; SOLAR-FLARES ; FILAMENT ERUPTIONS ; MAGNETIC-FIELDS ; ACTIVE REGIONS ; FLUX ROPES ; SYSTEMS ; PROMINENCES ; STABILITY ; EVOLUTION
Indexed BySCI
Language英语
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS IDWOS:000434264500002
PublisherIOP PUBLISHING LTD
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Document Type期刊论文
Identifierhttp://libir.pmo.ac.cn/handle/332002/24071
Collection中国科学院紫金山天文台
Corresponding AuthorWang, Ya
Affiliation1.Chinese Acad Sci, Purple Mt Observ, Key Lab Dark Matter & Space Sci, Nanjing 210008, Jiangsu, Peoples R China
2.Univ Chinese Acad Sci, Beijing 100049, Peoples R China
3.Univ Sci & Technol China, Sch Astron & Space Sci, Hefei 230026, Anhui, Peoples R China
4.Chinese Acad Sci, Xinjiang Astron Observ, Urumqi 830011, Peoples R China
5.Big Bear Solar Observ, Big Bear City, CA 92314 USA
Recommended Citation
GB/T 7714
Wang, Ya,Su, Yingna,Shen, Jinhua,et al. High-resolution He I 10830 angstrom Narrowband Imaging for an M-class Flare. II. Multiple Hot Channels: Their Origin and Destination[J]. ASTROPHYSICAL JOURNAL,2018,859(2):11.
APA Wang, Ya,Su, Yingna,Shen, Jinhua,Yang, Xu,Cao, Wenda,&Ji, Haisheng.(2018).High-resolution He I 10830 angstrom Narrowband Imaging for an M-class Flare. II. Multiple Hot Channels: Their Origin and Destination.ASTROPHYSICAL JOURNAL,859(2),11.
MLA Wang, Ya,et al."High-resolution He I 10830 angstrom Narrowband Imaging for an M-class Flare. II. Multiple Hot Channels: Their Origin and Destination".ASTROPHYSICAL JOURNAL 859.2(2018):11.
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