Evidence for the Formation of a Large-Scale Current Sheet in a Solar Flare

By L. Sui, Gordon D. Holman. 2003

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In Astronomy and Astrophysics

Citations in the corpus

Sixty-five years of solar radioastronomy: flares, coronal mass ejections and Sun–Earth connection (2008, background): “30 from Sui and Holman 2003).”
An Observational Overview of Solar Flares (2011, background): “We have evidence of magnetic field relaxation (Sui & Holman 2003) consistent with shrinkage beneath a reconnection region, in whichbetatron acceleration would occur (Somov & Kosugi 1997).”
Direct Observations of the Magnetic Reconnection Site of an Eruption on 2003 November 18 (2005, background): “…indirectly by observing the dynamic behavior of the products of magnetic reconnection: the separating flare ribbons on the solar surface (Poletto & Kopp 1986; Qiu et al. 2002; Wang et al. 2003; Qiu et al. 2004), the growing flare loops in the corona (Sui & Holman 2003; Sui et al. 2004), and so on.”
Coronal Mass Ejections: Observations (2012, background): “(2005) found considerable overlap of accelerations and speeds between the two CME groups. While flare-associated CMEs are generally faster than those without flares, there is also a correlation between CME speeds and flare X-ray peak fluxes, in which CMEs associated with the smaller flares are simil”
SIMULTANEOUS OBSERVATION OF RECONNECTION INFLOW AND OUTFLOW ASSOCIATED WITH THE 2010 AUGUST 18 SOLAR FLARE (2011, background): “…et al. 2001; Narukage & Shibata 2006; Li & Zhang 2009), reconnection outflows (Wang et al. 2007), supra-arcade downflows (McKenzie & Hudson 1999; Innes et al. 2003; Asai et al. 2004; Savage & McKenzie 2011), and current-sheet-like structures (Sui & Holman 2003; Lin et al. 2005; Liu et al. 2010).”
Double Coronal Hard and Soft X-Ray Source Observed by RHESSI: Evidence for Magnetic Reconnection and Particle Acceleration in Solar Flares (2007, background): “Energy Dependence of Source Structure The energy-dependent source morphology presented in §2.1 (see Figure 4, lower left) is similar to that reported by Sui & Holman (2003) and Sui et al. (2004) and interpreted as magnetic reconnection taking place between the two coronal sources.”
Recent Advances in Understanding Particle Acceleration Processes in Solar Flares (2011, methodology): “These are orders of magnitude smaller than the 108 - 1010 cm sizes associated with flares (Masuda et al. 1994; Sui & Holman 2003; Jiang et al. 2006).”
PLASMOID EJECTIONS AND LOOP CONTRACTIONS IN AN ERUPTIVE M7.7 SOLAR FLARE: EVIDENCE OF PARTICLE ACCELERATION AND HEATING IN MAGNETIC RECONNECTION OUTFLOWS (2013, background): “Another surprise has been the descent of the loop-top X-ray source at typically 10–40 kms−1 early in the impulsive phase before its common ascent through the decay phase (Sui & Holman 2003; Sui et al. 2004; Liu et al. 2004; Shen et al. 2008).”
RECONNECTION OUTFLOWS AND CURRENT SHEET OBSERVED WITH HINODE/XRT IN THE 2008 APRIL 9 “CARTWHEEL CME” FLARE (2010, methodology): “Reports of impulsive-phase RHESSI double coronal sources have been made by other authors (e.g. Liu et al. 2008; Sui, Holman, & Dennis 2004; Sui & Holman 2003) with the lower source corresponding to the top of the rising arcade and the upper source possibly corresponding to an ascending reconnection…”
Imaging coronal magnetic-field reconnection in a solar flare (2013, background): “RHESSI X-ray fluxes(30) are shown as red (blue) contours in the 4-10 (10-20) keV bands at 10, 40, and 80% of the maximum in each image.”
ELECTRON ACCELERATION BY MULTI-ISLAND COALESCENCE (2010, methodology): “Therefore, our simulation can probably be best applied to the solar flares which show evidence of very long current sheets (e.g. Sui & Holman 2003; Bemporad et al. 2006).”
Stochastic Acceleration by Turbulence (2012, background): “• In rare cases, when the FP sources are weak or occulted, one can see a double LT source (Figure 2 middle, from Liu et al. 2008; see also Sui & Holman, 2003) as expected in the model depicted on the left.”
Hard X-ray emission from the solar corona (2008, background): “The coronal source was stationary for several minutes and eventually moved outward at a speed of ≈300 km s−1 (Sui and Holman 2003).”
Observations of Turbulent Magnetic Reconnection within a Solar Current Sheet (2018, background): “…near the reconnection region (Yokoyama et al. 2001; Savage & McKenzie 2011; Takasao et al. 2012; Liu et al. 2013; Liu 2013; Xue et al. 2016), double hard X-ray coronal sources (Sui & Holman 2003), and changes of connectivity of coronal loops (Su et al. 2013; Yang et al. 2015; Li et al. 2016).”
Implications of X-ray Observations for Electron Acceleration and Propagation in Solar Flares (2011, background): “The centroid of the lower source is higher in altitude at higher X-ray energies, while the centroid of the upper source is lower in altitude at higher X-ray energies, indicating that energy release occurred between these coronal sources (Sui and Holman 2003; Sui et al. 2004; Liu et al. 2008, 2009b).”