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Title: Observations of Reconnection Flows in a Flare on the Solar Disk

Abstract

Magnetic reconnection is a well-accepted part of the theory of solar eruptive events, though the evidence is still circumstantial. Intrinsic to the reconnection picture of a solar eruptive event, particularly in the standard model for two-ribbon flares (CSHKP model), are an advective flow of magnetized plasma into the reconnection region, expansion of field above the reconnection region as a flux rope erupts, retraction of heated post-reconnection loops, and downflows of cooling plasma along those loops. We report on a unique set of Solar Dynamics Observatory /Atmospheric Imaging Assembly imaging and Hinode /EUV Imaging Spectrometer spectroscopic observations of the disk flare SOL2016-03-23T03:54 in which all four flows are present simultaneously. This includes spectroscopic evidence for a plasma upflow in association with large-scale expanding closed inflow field. The reconnection inflows are symmetric, and consistent with fast reconnection, and the post-reconnection loops show a clear cooling and deceleration as they retract. Observations of coronal reconnection flows are still rare, and most events are observed at the solar limb, obscured by complex foregrounds, making their relationship to the flare ribbons, cusp field, and arcades formed in the lower atmosphere difficult to interpret. The disk location and favorable perspective of this event have removed thesemore » ambiguities giving a clear picture of the reconnection dynamics.« less

Authors:
; ; ; ; ;  [1]
  1. SUPA, School of Physics and Astronomy, University of Glasgow, Glasgow G12 8QQ (United Kingdom)
Publication Date:
OSTI Identifier:
22654390
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astrophysical Journal Letters; Journal Volume: 847; Journal Issue: 1; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ACCELERATION; COOLING; EXPANSION; LIMBS; MAGNETIC RECONNECTION; MASS; PLASMA; SOLAR FLARES; SOLAR WIND; SPECTROMETERS; STANDARD MODEL; SUN; SYMMETRY; ULTRAVIOLET RADIATION

Citation Formats

Wang, Juntao, Simões, P. J. A., Jeffrey, N. L. S., Fletcher, L., Wright, P. J., and Hannah, I. G., E-mail: j.wang.4@research.gla.ac.uk. Observations of Reconnection Flows in a Flare on the Solar Disk. United States: N. p., 2017. Web. doi:10.3847/2041-8213/AA8904.
Wang, Juntao, Simões, P. J. A., Jeffrey, N. L. S., Fletcher, L., Wright, P. J., & Hannah, I. G., E-mail: j.wang.4@research.gla.ac.uk. Observations of Reconnection Flows in a Flare on the Solar Disk. United States. doi:10.3847/2041-8213/AA8904.
Wang, Juntao, Simões, P. J. A., Jeffrey, N. L. S., Fletcher, L., Wright, P. J., and Hannah, I. G., E-mail: j.wang.4@research.gla.ac.uk. Wed . "Observations of Reconnection Flows in a Flare on the Solar Disk". United States. doi:10.3847/2041-8213/AA8904.
@article{osti_22654390,
title = {Observations of Reconnection Flows in a Flare on the Solar Disk},
author = {Wang, Juntao and Simões, P. J. A. and Jeffrey, N. L. S. and Fletcher, L. and Wright, P. J. and Hannah, I. G., E-mail: j.wang.4@research.gla.ac.uk},
abstractNote = {Magnetic reconnection is a well-accepted part of the theory of solar eruptive events, though the evidence is still circumstantial. Intrinsic to the reconnection picture of a solar eruptive event, particularly in the standard model for two-ribbon flares (CSHKP model), are an advective flow of magnetized plasma into the reconnection region, expansion of field above the reconnection region as a flux rope erupts, retraction of heated post-reconnection loops, and downflows of cooling plasma along those loops. We report on a unique set of Solar Dynamics Observatory /Atmospheric Imaging Assembly imaging and Hinode /EUV Imaging Spectrometer spectroscopic observations of the disk flare SOL2016-03-23T03:54 in which all four flows are present simultaneously. This includes spectroscopic evidence for a plasma upflow in association with large-scale expanding closed inflow field. The reconnection inflows are symmetric, and consistent with fast reconnection, and the post-reconnection loops show a clear cooling and deceleration as they retract. Observations of coronal reconnection flows are still rare, and most events are observed at the solar limb, obscured by complex foregrounds, making their relationship to the flare ribbons, cusp field, and arcades formed in the lower atmosphere difficult to interpret. The disk location and favorable perspective of this event have removed these ambiguities giving a clear picture of the reconnection dynamics.},
doi = {10.3847/2041-8213/AA8904},
journal = {Astrophysical Journal Letters},
number = 1,
volume = 847,
place = {United States},
year = {Wed Sep 20 00:00:00 EDT 2017},
month = {Wed Sep 20 00:00:00 EDT 2017}
}