Non-damping oscillations at flaring loops
文献类型：期刊论文
| 作者 | 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 |
| 刊名 | ASTRONOMY & ASTROPHYSICS
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| 出版日期 | 2018-09-25 |
| 卷号 | 617页码:9 |
| ISSN号 | 1432-0746 |
| 关键词 | Sun: flares Sun: oscillations Sun: UV radiation Sun: X-rays, gamma rays line: profiles techniques: spectroscopic |
| DOI | 10.1051/0004-6361/201832991 |
| 通讯作者 | Li, D.(lidong@pmo.ac.cn) |
| 英文摘要 | Context. 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. |
| WOS关键词 | QUASI-PERIODIC PULSATIONS ; REGION-IMAGING-SPECTROGRAPH ; DOPPLER-SHIFT OSCILLATIONS ; X-RAY-EMISSION ; SOLAR-FLARE ; CORONAL LOOPS ; TRANSVERSE OSCILLATIONS ; TRANSITION-REGION ; MAGNETIC-FIELDS ; ACTIVE-REGION |
| WOS研究方向 | Astronomy & Astrophysics |
| 语种 | 英语 |
| 出版者 | EDP SCIENCES S A |
| WOS记录号 | WOS:000445446100001 |
| 源URL | [http://libir.pmo.ac.cn/handle/332002/21348]  |
| 专题 | 中国科学院紫金山天文台 |
| 通讯作者 | Li, D. |
| 作者单位 | 1.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 |
| 推荐引用方式 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. |
入库方式： OAI收割
来源：紫金山天文台
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