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Dark feature in EUV post-flare loops

Published online by Cambridge University Press:  09 September 2016

Qiao Song ,
Mei Zhang ,
Jing-Song Wang ,
Xue-Shang Feng  and
Xiao-Xin Zhang
Qiao Song
Affiliation:
Key Laboratory of Space Weather, National Center for Space Weather, China Meteorological Administration, Beijing 100081, China. email: [email protected] State Key Laboratory of Space Weather, National Space Science Center, Chinese Academy of Sciences, Beijing 100190, China Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China
Mei Zhang
Affiliation:
Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China
Jing-Song Wang
Affiliation:
Key Laboratory of Space Weather, National Center for Space Weather, China Meteorological Administration, Beijing 100081, China. email: [email protected]
Xue-Shang Feng
Affiliation:
State Key Laboratory of Space Weather, National Space Science Center, Chinese Academy of Sciences, Beijing 100190, China
Xiao-Xin Zhang
Affiliation:
Key Laboratory of Space Weather, National Center for Space Weather, China Meteorological Administration, Beijing 100081, China. email: [email protected]
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Abstract

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Post-flare loops (PFLs) usually appear in the late phase of eruptive flares as an arcade-like loop system. The Atmospheric Imaging Assembly (AIA) on-board the Solar Dynamics Observatory (SDO) delivers continuously high temporal and spatial resolution extreme ultraviolet (EUV) observations, providing a unique chance to study the PFLs. In this work, we use SDO/AIA high-quality EUV images to study the dark loop-like features in post-flare loops (DPFLs) of an X5.4 flare. Our analysis shows that: 1) the DPFLs are darker than their surrounding and the bright loops, but are brighter than the EUV background; 2) the DPFLs appear in multiple EUV channels, which indicates that they are absorption features; 3) the DPFLs are associated with downflows that are caused by the thermal instability in the cooling process of the flare.

Keywords

Solar flarePost-flare loop
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , Symposium S320: Solar and Stellar Flares and their Effects on Planets , August 2015 , pp. 95 - 97
Copyright
Copyright © International Astronomical Union 2016 

References

Anzer, U. & Heinzel, P. 2005, ApJ, 622, 714 CrossRefGoogle Scholar
Bruzek, A. 1964, ApJ, 140, 746 Google Scholar
Forbes, T. G. & Acton, L. W. 1996, ApJ, 459, 330 CrossRefGoogle Scholar
Kahler, S. 1977, ApJ, 214, 891 Google Scholar
Lemen, J. R., Title, A. M., & Akin, D. J., et al. 2012, Solar Physics, 275, 17 CrossRefGoogle Scholar
Pesnell, W. D., Thompson, B. J., & Chamberlin, P. C. 2012, Solar Physics, 275, 3 Google Scholar
Priest, E. R. & Forbes, T. G. 2002, A&A Rev., 10, 313 Google Scholar
Schrijver, C. J., De Rosa, M. L., & Metcalf, T., et al. 2008, ApJ, 675, 1637 Google Scholar
Sheeley, N. R. Jr., Bohlin, J. D., & Brueckner, G. E., et al. 1975, Solar Physics, 45, 377 Google Scholar
Song, Q., Zhang, J., Yang, S. H., & Liu, Y. 2013, Research in Astronomy and Astrophysics, 13, 226 CrossRefGoogle Scholar