Journal
ASTROPHYSICAL JOURNAL
Volume 722, Issue 1, Pages 329-342Publisher
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/722/1/329
Keywords
magnetic reconnection; Sun: corona; Sun: coronal mass ejections (CMEs); Sun: flares; Sun: magnetic topology; Sun: X-rays, gamma rays
Categories
Funding
- NASA [NNM07AA02C0, NNX08AG44G]
- NSF SHINE [ATM-0752257]
- NSF [ATM-0837841]
- Div Atmospheric & Geospace Sciences
- Directorate For Geosciences [0837841] Funding Source: National Science Foundation
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Supra-arcade downflows (SADs) have been observed with Yohkoh/SXT (soft X-rays (SXR)), TRACE (extreme ultraviolet (EUV)), SOHO/LASCO (white light), SOHO/SUMER (EUV spectra), and Hinode/XRT (SXR). Characteristics such as low emissivity and trajectories, which slow as they reach the top of the arcade, are consistent with post-reconnection magnetic flux tubes retracting from a reconnection site high in the corona until they reach a lower-energy magnetic configuration. Viewed from a perpendicular angle, SADs should appear as shrinking loops rather than downflowing voids. We present X-ray Telescope (XRT) observations of supra-arcade downflowing loops (SADLs) following a coronal mass ejection (CME) on 2008 April 9 and show that their speeds and decelerations are consistent with those determined for SADs. We also present evidence for a possible current sheet observed during this flare that extends between the flare arcade and the CME. Additionally, we show a correlation between reconnection outflows observed with XRT and outgoing flows observed with LASCO.
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