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Title: Imaging Observations of Magnetic Reconnection in a Solar Eruptive Flare

Abstract

Solar flares are among the most energetic events in the solar atmosphere. It is widely accepted that flares are powered by magnetic reconnection in the corona. An eruptive flare is usually accompanied by a coronal mass ejection, both of which are probably driven by the eruption of a magnetic flux rope (MFR). Here we report an eruptive flare on 2016 March 23 observed by the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory . The extreme-ultraviolet imaging observations exhibit the clear rise and eruption of an MFR. In particular, the observations reveal solid evidence of magnetic reconnection from both the corona and chromosphere during the flare. Moreover, weak reconnection is observed before the start of the flare. We find that the preflare weak reconnection is of tether-cutting type and helps the MFR to rise slowly. Induced by a further rise of the MFR, strong reconnection occurs in the rise phases of the flare, which is temporally related to the MFR eruption. We also find that the magnetic reconnection is more of 3D-type in the early phase, as manifested in a strong-to-weak shear transition in flare loops, and becomes more 2D-like in the later phase, as shown by the apparentmore » rising motion of an arcade of flare loops.« less

Authors:
;  [1];  [2];  [3];  [4]
  1. School of Astronomy and Space Science, Nanjing University, Nanjing 210023 (China)
  2. W. W. Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA 94305 (United States)
  3. Department of Physics, Montana State University, Bozeman, MT 59717 (United States)
  4. School of Mathematics and Statistics, University of St Andrews, Fife KY16 9SS, Scotland (United Kingdom)
Publication Date:
OSTI Identifier:
22663932
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astrophysical Journal; Journal Volume: 835; Journal Issue: 2; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; CHROMOSPHERE; ERUPTION; EXTREME ULTRAVIOLET RADIATION; MAGNETIC FLUX; MAGNETIC RECONNECTION; MASS; SOLAR FLARES; SOLIDS; SUN

Citation Formats

Li, Y., Ding, M. D., Sun, X., Qiu, J., and Priest, E. R., E-mail: yingli@nju.edu.cn. Imaging Observations of Magnetic Reconnection in a Solar Eruptive Flare. United States: N. p., 2017. Web. doi:10.3847/1538-4357/835/2/190.
Li, Y., Ding, M. D., Sun, X., Qiu, J., & Priest, E. R., E-mail: yingli@nju.edu.cn. Imaging Observations of Magnetic Reconnection in a Solar Eruptive Flare. United States. doi:10.3847/1538-4357/835/2/190.
Li, Y., Ding, M. D., Sun, X., Qiu, J., and Priest, E. R., E-mail: yingli@nju.edu.cn. Wed . "Imaging Observations of Magnetic Reconnection in a Solar Eruptive Flare". United States. doi:10.3847/1538-4357/835/2/190.
@article{osti_22663932,
title = {Imaging Observations of Magnetic Reconnection in a Solar Eruptive Flare},
author = {Li, Y. and Ding, M. D. and Sun, X. and Qiu, J. and Priest, E. R., E-mail: yingli@nju.edu.cn},
abstractNote = {Solar flares are among the most energetic events in the solar atmosphere. It is widely accepted that flares are powered by magnetic reconnection in the corona. An eruptive flare is usually accompanied by a coronal mass ejection, both of which are probably driven by the eruption of a magnetic flux rope (MFR). Here we report an eruptive flare on 2016 March 23 observed by the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory . The extreme-ultraviolet imaging observations exhibit the clear rise and eruption of an MFR. In particular, the observations reveal solid evidence of magnetic reconnection from both the corona and chromosphere during the flare. Moreover, weak reconnection is observed before the start of the flare. We find that the preflare weak reconnection is of tether-cutting type and helps the MFR to rise slowly. Induced by a further rise of the MFR, strong reconnection occurs in the rise phases of the flare, which is temporally related to the MFR eruption. We also find that the magnetic reconnection is more of 3D-type in the early phase, as manifested in a strong-to-weak shear transition in flare loops, and becomes more 2D-like in the later phase, as shown by the apparent rising motion of an arcade of flare loops.},
doi = {10.3847/1538-4357/835/2/190},
journal = {Astrophysical Journal},
number = 2,
volume = 835,
place = {United States},
year = {Wed Feb 01 00:00:00 EST 2017},
month = {Wed Feb 01 00:00:00 EST 2017}
}