NAOC Open IR
Spectroscopic observations of a flare-related coronal jet
Zhang, Q. M.1,3; Huang, Z. H.2; Hou, Y. J.3,4; Li, D.3; Ning, Z. J.1; Wu, Z.2
2021-03-17
Source PublicationASTRONOMY & ASTROPHYSICS
ISSN0004-6361
Volume647Pages:10
AbstractContext. Coronal jets are ubiquitous in active regions and coronal holes.Aims. In this paper, we study a coronal jet related to a C3.4 circular-ribbon flare in the active region 12434 on 2015 October 16.Methods. The flare and jet were observed in ultraviolet and extreme ultraviolet wavelengths by the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory (SDO). The line-of-sight magnetograms of the photosphere were observed by the Helioseismic and Magnetic Imager on board SDO. The whole event was covered by the Interface Region Imaging Spectrograph during its imaging and spectroscopic observations. Soft X-ray fluxes of the flare were recorded by the GOES spacecraft. Hard X-ray (HXR) fluxes at 4-50 keV were obtained from observations of RHESSI and Fermi. Radio dynamic spectra of the flare were recorded by the ground-based stations belonging to the e-Callisto network.Results. Two minifilaments were located under a 3D fan-spine structure before flare. The flare was generated by the eruption of one filament. The kinetic evolution of the jet was divided into two phases: a slow rise phase at a speed of similar to 131 km s(-1) and a fast rise phase at a speed of similar to 363 km s(-1) in the plane-of-sky. The slow rise phase may correspond to the impulsive reconnection at the breakout current sheet. The fast rise phase may correspond to magnetic reconnection at the flare current sheet. The transition between the two phases occurred at similar to 09:00:40 UT. The blueshifted Doppler velocities of the jet in the SiIV 1402.80 angstrom line range from -34 to -120 km s(-1). The accelerated high-energy electrons are composed of three groups. Those propagating upward along the open field generate type III radio bursts, while those propagating downward produce HXR emissions and drive chromospheric condensation observed in the SiIV line. The electrons trapped in the rising filament generate a microwave burst lasting for <= 40 s. Bidirectional outflows at the base of jet are manifested by significant line broadenings of the SiIV line. The blueshifted Doppler velocities of outflows range from -13 to -101 km s(-1). The redshifted Doppler velocities of outflows range from similar to 17 to similar to 170 km s(-1).Conclusions. Our multiwavelength observations of the flare-related jet are in favor of the breakout jet model and are important for understanding the acceleration and transport of nonthermal electrons.
Keywordline: profiles magnetic reconnection Sun: flares Sun: filaments prominences Sun: UV radiation
Funding OrganizationNSFC ; NSFC ; International Cooperation and Interchange Program ; International Cooperation and Interchange Program ; Youth Innovation Promotion Association CAS ; Youth Innovation Promotion Association CAS ; CAS Key Laboratory of Solar Activity ; CAS Key Laboratory of Solar Activity ; National Astronomical Observatories ; National Astronomical Observatories ; Specialized Research Fund for State Key Laboratories ; Specialized Research Fund for State Key Laboratories ; NSFC ; NSFC ; International Cooperation and Interchange Program ; International Cooperation and Interchange Program ; Youth Innovation Promotion Association CAS ; Youth Innovation Promotion Association CAS ; CAS Key Laboratory of Solar Activity ; CAS Key Laboratory of Solar Activity ; National Astronomical Observatories ; National Astronomical Observatories ; Specialized Research Fund for State Key Laboratories ; Specialized Research Fund for State Key Laboratories ; NSFC ; NSFC ; International Cooperation and Interchange Program ; International Cooperation and Interchange Program ; Youth Innovation Promotion Association CAS ; Youth Innovation Promotion Association CAS ; CAS Key Laboratory of Solar Activity ; CAS Key Laboratory of Solar Activity ; National Astronomical Observatories ; National Astronomical Observatories ; Specialized Research Fund for State Key Laboratories ; Specialized Research Fund for State Key Laboratories ; NSFC ; NSFC ; International Cooperation and Interchange Program ; International Cooperation and Interchange Program ; Youth Innovation Promotion Association CAS ; Youth Innovation Promotion Association CAS ; CAS Key Laboratory of Solar Activity ; CAS Key Laboratory of Solar Activity ; National Astronomical Observatories ; National Astronomical Observatories ; Specialized Research Fund for State Key Laboratories ; Specialized Research Fund for State Key Laboratories
DOI10.1051/0004-6361/202038924
Language英语
Funding ProjectNSFC[11773079] ; NSFC[11790302] ; NSFC[U1831112] ; NSFC[11903050] ; NSFC[11790304] ; NSFC[11973092] ; NSFC[11573072] ; NSFC[11703017] ; International Cooperation and Interchange Program[11961131002] ; Youth Innovation Promotion Association CAS ; CAS Key Laboratory of Solar Activity ; National Astronomical Observatories[KLSA202003] ; National Astronomical Observatories[KLSA202006] ; Specialized Research Fund for State Key Laboratories
Funding OrganizationNSFC ; NSFC ; International Cooperation and Interchange Program ; International Cooperation and Interchange Program ; Youth Innovation Promotion Association CAS ; Youth Innovation Promotion Association CAS ; CAS Key Laboratory of Solar Activity ; CAS Key Laboratory of Solar Activity ; National Astronomical Observatories ; National Astronomical Observatories ; Specialized Research Fund for State Key Laboratories ; Specialized Research Fund for State Key Laboratories ; NSFC ; NSFC ; International Cooperation and Interchange Program ; International Cooperation and Interchange Program ; Youth Innovation Promotion Association CAS ; Youth Innovation Promotion Association CAS ; CAS Key Laboratory of Solar Activity ; CAS Key Laboratory of Solar Activity ; National Astronomical Observatories ; National Astronomical Observatories ; Specialized Research Fund for State Key Laboratories ; Specialized Research Fund for State Key Laboratories ; NSFC ; NSFC ; International Cooperation and Interchange Program ; International Cooperation and Interchange Program ; Youth Innovation Promotion Association CAS ; Youth Innovation Promotion Association CAS ; CAS Key Laboratory of Solar Activity ; CAS Key Laboratory of Solar Activity ; National Astronomical Observatories ; National Astronomical Observatories ; Specialized Research Fund for State Key Laboratories ; Specialized Research Fund for State Key Laboratories ; NSFC ; NSFC ; International Cooperation and Interchange Program ; International Cooperation and Interchange Program ; Youth Innovation Promotion Association CAS ; Youth Innovation Promotion Association CAS ; CAS Key Laboratory of Solar Activity ; CAS Key Laboratory of Solar Activity ; National Astronomical Observatories ; National Astronomical Observatories ; Specialized Research Fund for State Key Laboratories ; Specialized Research Fund for State Key Laboratories
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS IDWOS:000630014200006
PublisherEDP SCIENCES S A
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Document Type期刊论文
Identifierhttp://ir.bao.ac.cn/handle/114a11/78690
Collection中国科学院国家天文台
Corresponding AuthorZhang, Q. M.
Affiliation1.Chinese Acad Sci, Key Lab Dark Matter & Space Astron, Purple Mt Observ, Nanjing 210023, Peoples R China
2.Shandong Univ, Inst Space Sci, Shandong Prov Key Lab Opt Astron & Solar Terr E, Weihai 264209, Peoples R China
3.Chinese Acad Sci, CAS Key Lab Solar Activ, Natl Astron Observ, Beijing 100101, Peoples R China
4.Univ Chinese Acad Sci, Sch Astron & Space Sci, Beijing 100049, Peoples R China
Recommended Citation
GB/T 7714
Zhang, Q. M.,Huang, Z. H.,Hou, Y. J.,et al. Spectroscopic observations of a flare-related coronal jet[J]. ASTRONOMY & ASTROPHYSICS,2021,647:10.
APA Zhang, Q. M.,Huang, Z. H.,Hou, Y. J.,Li, D.,Ning, Z. J.,&Wu, Z..(2021).Spectroscopic observations of a flare-related coronal jet.ASTRONOMY & ASTROPHYSICS,647,10.
MLA Zhang, Q. M.,et al."Spectroscopic observations of a flare-related coronal jet".ASTRONOMY & ASTROPHYSICS 647(2021):10.
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