NAOC Open IR  > 射电天文研究部
Doppler Shift Oscillations from a Hot Line Observed by IRIS
Li, D.1,2,3; Ning, Z. J.1; Huang, Y.1; Chen, N. -H.4; Zhang, Q. M.1; Su, Y. N.1; Su, W.1,2
2017-11-10
Source PublicationASTROPHYSICAL JOURNAL
Volume849Issue:2
AbstractWe present a detailed investigation of the Doppler shift oscillations in a hot loop during an M7.1 flare on 2014 October 27 observed by the Interface Region Imaging Spectrograph. The periodic oscillations are observed in the Doppler shift of Fe XXI. 1354.09 angstrom (log T similar to 7.05), and the dominant period is about 3.1. minutes. However, such 3.1 minute oscillations are not found in the line-integrated intensity of Fe XXI. 1354.09 angstrom, AIA EUV fluxes, or microwave emissions. Solar Dynamics Observatory/AIA and Hinode/XRT imaging observations indicate that the Doppler shift oscillations locate at the hot loop-top region (>= 11 MK). Moreover, the differential emission measure results show that the temperature is increasing rapidly when the Doppler shift oscillates, but the number density does not exhibit the corresponding increases nor oscillations, implying that the flare loop is likely to oscillate in an incompressible mode. All of these facts suggest that the Doppler shift oscillations at the shorter period are most likely the standing kink oscillations in a flare loop. Meanwhile, a longer period of about 10. minutes is identified in the time series of Doppler shift and line-integrated intensity, GOES SXR fluxes, and AIA EUV light curves, indicating the periodic energy release in this flare, which may be caused by a slow mode wave.
SubtypeArticle
KeywordLine: Profiles Sun: Flares Sun: Oscillations Sun: Uv Radiation
WOS HeadingsScience & Technology ; Physical Sciences
Funding OrganizationNSFC(11603077 ; NSFC(11603077 ; 973 program(2014CB744200 ; 973 program(2014CB744200 ; Youth Fund of Jiangsu(BK20161095 ; Youth Fund of Jiangsu(BK20161095 ; Chinese Academy of Sciences ; Chinese Academy of Sciences ; International Space Science Institute in Beijing (ISSI-BJ) ; International Space Science Institute in Beijing (ISSI-BJ) ; Surface Project of Jiangsu(BK 20161618) ; Surface Project of Jiangsu(BK 20161618) ; Youth Innovation Promotion Association CAS ; Youth Innovation Promotion Association CAS ; 11573072 ; 11573072 ; 2010DP173032) ; 2010DP173032) ; BK20171108 ; BK20171108 ; 11773079 ; 11773079 ; BK20141043) ; BK20141043) ; 11773061 ; 11773061 ; 11473071 ; 11473071 ; 11333009 ; 11333009 ; XDA15052200 ; XDA15052200 ; KLSA201708) ; KLSA201708) ; NSFC(11603077 ; NSFC(11603077 ; 973 program(2014CB744200 ; 973 program(2014CB744200 ; Youth Fund of Jiangsu(BK20161095 ; Youth Fund of Jiangsu(BK20161095 ; Chinese Academy of Sciences ; Chinese Academy of Sciences ; International Space Science Institute in Beijing (ISSI-BJ) ; International Space Science Institute in Beijing (ISSI-BJ) ; Surface Project of Jiangsu(BK 20161618) ; Surface Project of Jiangsu(BK 20161618) ; Youth Innovation Promotion Association CAS ; Youth Innovation Promotion Association CAS ; 11573072 ; 11573072 ; 2010DP173032) ; 2010DP173032) ; BK20171108 ; BK20171108 ; 11773079 ; 11773079 ; BK20141043) ; BK20141043) ; 11773061 ; 11773061 ; 11473071 ; 11473071 ; 11333009 ; 11333009 ; XDA15052200 ; XDA15052200 ; KLSA201708) ; KLSA201708)
DOI10.3847/1538-4357/aa9073
WOS KeywordCORONAL LOOP OSCILLATIONS ; HARD X-RAY ; QUASI-PERIODIC PULSATIONS ; SOLAR-FLARE LOOPS ; REGION-IMAGING-SPECTROGRAPH ; BRAGG CRYSTAL SPECTROMETER ; TRANSVERSE OSCILLATIONS ; MAGNETIC RECONNECTION ; TIME-SERIES ; WAVES
Indexed BySCI
Language英语
Funding OrganizationNSFC(11603077 ; NSFC(11603077 ; 973 program(2014CB744200 ; 973 program(2014CB744200 ; Youth Fund of Jiangsu(BK20161095 ; Youth Fund of Jiangsu(BK20161095 ; Chinese Academy of Sciences ; Chinese Academy of Sciences ; International Space Science Institute in Beijing (ISSI-BJ) ; International Space Science Institute in Beijing (ISSI-BJ) ; Surface Project of Jiangsu(BK 20161618) ; Surface Project of Jiangsu(BK 20161618) ; Youth Innovation Promotion Association CAS ; Youth Innovation Promotion Association CAS ; 11573072 ; 11573072 ; 2010DP173032) ; 2010DP173032) ; BK20171108 ; BK20171108 ; 11773079 ; 11773079 ; BK20141043) ; BK20141043) ; 11773061 ; 11773061 ; 11473071 ; 11473071 ; 11333009 ; 11333009 ; XDA15052200 ; XDA15052200 ; KLSA201708) ; KLSA201708) ; NSFC(11603077 ; NSFC(11603077 ; 973 program(2014CB744200 ; 973 program(2014CB744200 ; Youth Fund of Jiangsu(BK20161095 ; Youth Fund of Jiangsu(BK20161095 ; Chinese Academy of Sciences ; Chinese Academy of Sciences ; International Space Science Institute in Beijing (ISSI-BJ) ; International Space Science Institute in Beijing (ISSI-BJ) ; Surface Project of Jiangsu(BK 20161618) ; Surface Project of Jiangsu(BK 20161618) ; Youth Innovation Promotion Association CAS ; Youth Innovation Promotion Association CAS ; 11573072 ; 11573072 ; 2010DP173032) ; 2010DP173032) ; BK20171108 ; BK20171108 ; 11773079 ; 11773079 ; BK20141043) ; BK20141043) ; 11773061 ; 11773061 ; 11473071 ; 11473071 ; 11333009 ; 11333009 ; XDA15052200 ; XDA15052200 ; KLSA201708) ; KLSA201708)
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS IDWOS:000414725900009
Citation statistics
Document Type期刊论文
Identifierhttp://ir.bao.ac.cn/handle/114a11/20214
Collection射电天文研究部
Affiliation1.Chinese Acad Sci, Key Lab Dark Matter & Space Astron, Purple Mt Observ, Nanjing 210008, Jiangsu, Peoples R China
2.Nanjing Univ, Minist Educ, Key Lab Modern Astron & Astrophys, Nanjing 210023, Jiangsu, Peoples R China
3.Natl Astron Observ, CAS Key Lab Solar Act, Beijing 100012, Peoples R China
4.Korea Astron & Space Sci Inst, Daejeon 34055, South Korea
Recommended Citation
GB/T 7714
Li, D.,Ning, Z. J.,Huang, Y.,et al. Doppler Shift Oscillations from a Hot Line Observed by IRIS[J]. ASTROPHYSICAL JOURNAL,2017,849(2).
APA Li, D..,Ning, Z. J..,Huang, Y..,Chen, N. -H..,Zhang, Q. M..,...&Su, W..(2017).Doppler Shift Oscillations from a Hot Line Observed by IRIS.ASTROPHYSICAL JOURNAL,849(2).
MLA Li, D.,et al."Doppler Shift Oscillations from a Hot Line Observed by IRIS".ASTROPHYSICAL JOURNAL 849.2(2017).
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