RECONNECTION OUTFLOWS AND CURRENT SHEET OBSERVED WITH HINODE/XRT IN THE 2008 APRIL 9 “CARTWHEEL CME” FLARE

By S. Savage, D. McKenzie, K. Reeves, T. Forbes, D. Longcope. 2010

132 citations recorded by the source corpus.

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.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/05a4067162703208ac3dd27002c2bdadcbb5f263

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In Astronomy and Astrophysics

1. S. Patsourakos
2. A. Vourlidas
3. Xin Cheng
4. Guillermo Stenborg
5. M. Ding
6. Nat Gopalswamy
7. R. Howard
8. M. Temmer

Citations in the corpus

• DIRECT EVIDENCE FOR A FAST CORONAL MASS EJECTION DRIVEN BY THE PRIOR FORMATION AND SUBSEQUENT DESTABILIZATION OF A MAGNETIC FLUX ROPE (2012, background): “Moreover, SXT and XRT observations showed evidence of cusp-shaped loops forming under the erupting flux which sometimes has a concave upwards V-shape (e.g., Tsuneta et al. 1992; Tsuneta 1997; Savage et al. 2010).”
• Observations of Turbulent Magnetic Reconnection within a Solar Current Sheet (2018, background): “…sheet are mostly limited by the wavelength window that only responds to relatively narrow and low temperatures and/or the field of view that is not large enough (Lin et al. 2005, 2009; Ciaravella et al. 2003; Ciaravella & Raymond 2008; Savage et al. 2010; Ling et al. 2014; Seaton et al. 2017).”