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Non-damping oscillations at flaring loops
Li, D.1,2,3; Yuan, D.4; Su, Y. N.1,5; Zhang, Q. M.1,3; Su, W.6; Ning, Z. J.1,5
2018-09-25
Source PublicationASTRONOMY & ASTROPHYSICS
ISSN1432-0746
Volume617Pages:9
Corresponding AuthorLi, D.(lidong@pmo.ac.cn)
AbstractContext. Quasi-periodic oscillations are usually detected as spatial displacements of coronal loops in imaging observations or as periodic shifts of line properties (i.e., Doppler velocity, line width and intensity) in spectroscopic observations. They are often applied for remote diagnostics of magnetic fields and plasma properties on the Sun. Aims. We combine the imaging and spectroscopic measurements of available space missions, and investigate the properties of non-damping oscillations at flaring loops. Methods. We used the Interface Region Imaging Spectrograph (IRIS) to measure the spectrum over a narrow slit. The double-component Gaussian fitting method was used to extract the line profile of Fe xxi 1354.08 angstrom at the "OI" spectral window. The quasi-periodicity of loop oscillations were identified in the Fourier and wavelet spectra. Results. A periodicity at about 40 s is detected in the line properties of Fe xxi 1354.08 angstrom, hard X-ray emissions in GOES 1-8 angstrom derivative, and Fermi 26-50 keV. The Doppler velocity and line width oscillate in phase, while a phase shift of about pi/2 is detected between the Doppler velocity and peak intensity. The amplitudes of Doppler velocity and line width oscillation are about 2.2 km s(-1) and 1.9 km s(-1), respectively, while peak intensity oscillates with amplitude at about 3.6% of the background emission. Meanwhile, a quasi-period of about 155 s is identified in the Doppler velocity and peak intensity of the Fe xxi 1354.08 angstrom line emission, and AIA 131 angstrom intensity. Conclusions. The oscillations at about 40 s are not damped significantly during the observation; this might be linked to the global kink modes of flaring loops. The periodicity at about 155 s is most likely a signature of recurring downflows after chromospheric evaporation along flaring loops. The magnetic field strengths of the flaring loops are estimated to be about 120-170 G using the magnetohydrodynamic seismology diagnostics, which are consistent with the magnetic field modeling results using the flux rope insertion method.
KeywordSun: flares Sun: oscillations Sun: UV radiation Sun: X-rays, gamma rays line: profiles techniques: spectroscopic
DOI10.1051/0004-6361/201832991
WOS KeywordQUASI-PERIODIC PULSATIONS ; REGION-IMAGING-SPECTROGRAPH ; DOPPLER-SHIFT OSCILLATIONS ; X-RAY-EMISSION ; SOLAR-FLARE ; CORONAL LOOPS ; TRANSVERSE OSCILLATIONS ; TRANSITION-REGION ; MAGNETIC-FIELDS ; ACTIVE-REGION
Indexed BySCI
Language英语
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS IDWOS:000445446100001
PublisherEDP SCIENCES S A
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Document Type期刊论文
Identifierhttp://libir.pmo.ac.cn/handle/332002/21349
Collection中国科学院紫金山天文台
Corresponding AuthorLi, D.
Affiliation1.Chinese Acad Sci, Key Lab Dark Matter & Space Sci, Purple Mt Observ, Nanjing 210034, Jiangsu, Peoples R China
2.Chinese Acad Sci, Sate Key Lab Space Weather, Beijing 100190, Peoples R China
3.Natl Astron Observ, CAS Key Lab Solar Act, Beijing 100012, Peoples R China
4.Harbin Inst Technol, Inst Space Sci & Appl Technol, Shenzhen Campus, Shenzhen 518055, Peoples R China
5.Univ Sci & Technol China, Sch Astron & Space Sci, Hefei 230026, Anhui, Peoples R China
6.Huazhong Univ Sci & Technol, Sch Phys, MOE Key Lab Fundamental Phys Quant Measurements, Wuhan 430074, Hubei, Peoples R China
Recommended Citation
GB/T 7714
Li, D.,Yuan, D.,Su, Y. N.,et al. Non-damping oscillations at flaring loops[J]. ASTRONOMY & ASTROPHYSICS,2018,617:9.
APA Li, D.,Yuan, D.,Su, Y. N.,Zhang, Q. M.,Su, W.,&Ning, Z. J..(2018).Non-damping oscillations at flaring loops.ASTRONOMY & ASTROPHYSICS,617,9.
MLA Li, D.,et al."Non-damping oscillations at flaring loops".ASTRONOMY & ASTROPHYSICS 617(2018):9.
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