Direct Observations of the Magnetic Reconnection Site of an Eruption on 2003 November 18

Lin, Jin‐Ming; Ko, YK; Sui, Linhui; Raymond, J. C.; Stenborg, G.; YC, Jiang; Zhao, Shiqing; Mancuso, Salvatore

doi:10.1086/428110

Cited by 305 publications

(352 citation statements)

References 38 publications

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“…Because the timescale of reconnection is long compared to the timescale of the onset stage (Alfvén timescale), a long CS would be expected in the eruption even though reconnection is considered fast. The highest altitude flare loops reach and the distance that the rear part of the CME propagates during the typical eruptive event have indirectly confirmed the formation of the long CS (see discussions of Ciaravella et al 2002;Lin 2002;Ko et al 2003;Lin et al 2005).…”

Section: Have Convincingly Showed That Both the Reconnection Sites Comentioning

confidence: 83%

“…Ko et al (2003) studied the emission features and properties of the CS in detail, identified several plasma blobs flowing away from the Sun along the CS and measured the speed of the reconnection outflow and the rate of magnetic reconnection as well as the magnetic field strength near the CS. Lin et al (2005) performed direct measurement of the reconnection inflow speed near the CS, identified five moving plasma blobs to obtain the reconnection outflow speed and the rate of reconnection. McKenzie and Hudson (1999), Innes et al (2003aInnes et al ( , 2003b, Asai et al (2004), Sheeley et al (2004), Reeves et al (2008a), and Savage and McKenzie (2011) studied the sunward reconnection outflow above the flare loops and recognized fine structures of the plasma flow, also known as the supra-arcade downflow (SAD).…”

Section: Have Convincingly Showed That Both the Reconnection Sites Comentioning

confidence: 99%

“…In the spirit of works by and Ko et al (2003), Lin et al (2005) looked into various aspects of an event taking place on November 18, 2003. The event started with a rapid expansion of a few magnetic arcades located over the east limb of the Sun and developed an energetic partial-halo CME, a long CS, and a group of bright flare loops in the wake of the CME.…”

Section: The Reconnection Inflow Near the Current Sheetmentioning

confidence: 99%

“…It was observed by several instruments, both in space and image was taken at 10:26 UT and has been enhanced by the wavelet technique in order to emphasize the morphological features at various positions of the CME, the EIT 195 Å image was taken at 10:14 UT, the left UVCS image was made by stacking five UVCS exposures in Lyα that were taken at an altitude of 1.70 R and cover the time interval from 10:04 UT (right edge) to 10:14 UT (left edge), and the right UVCS image was made by stacking four UVCS exposures in Lyα that were taken at an altitude of 1.52 R and cover the time interval from 10:17 UT (right edge) to 10:23 UT (left edge). From Lin et al (2005) on the ground, including EIT, UVCS, and LASCO on board the SOHO, the RHESSI, and the MLSO MK-4 coronameter. Lin et al (2005) combined the data from these instruments to investigate various properties of the eruptive process, including those around the CS.…”

Section: The Reconnection Inflow Near the Current Sheetmentioning

confidence: 99%

“…From Lin et al (2005) on the ground, including EIT, UVCS, and LASCO on board the SOHO, the RHESSI, and the MLSO MK-4 coronameter. Lin et al (2005) combined the data from these instruments to investigate various properties of the eruptive process, including those around the CS. The maximum velocities of the CME leading edge and the core were 1939 and 1484 km s −1 , respectively.…”

Section: The Reconnection Inflow Near the Current Sheetmentioning

confidence: 99%

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Review on Current Sheets in CME Development: Theories and Observations

et al. 2015

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We introduce how the catastrophe model for solar eruptions predicted the formation and development of the long current sheet (CS) and how the observations were used to recognize the CS at the place where the CS is presumably located. Then, we discuss the direct measurement of the CS region thickness by studying the brightness distribution of the CS region at different wavelengths. The thickness ranges from 10 4 km to about 10 5 km at heights between 0.27 and 1.16 R from the solar surface. But the traditional theory indicates that the CS is as thin as the proton Larmor radius, which is of order tens of meters in the corona. We look into the huge difference in the thickness between observations and theoretical expectations. The possible impacts that affect measurements and results are studied, and physical causes leading to a thick CS region in which reconnection can still occur at a reasonably fast rate are analyzed. Studies in both theories and observations suggest that the difference between the true value and the apparent value of the CS thickness is not significant as long as the CS could be recognised in observations. We review observations that show complex structures and flows inside the CS region and present recent numerical modelling results on some aspects of these structures. Both observations and numerical experiments indicate that the downward reconnection outflows are usually slower than the upward ones in the same eruptive event. Numerical simulations show that the complex structure inside CS and its temporal behavior as a result of turbulence and the Petschek-type slow-mode shock could probably account for the thick CS and fast reconnection. But whether the CS itself is that thick still remains unknown since, for the time being, we cannot measure the electric current directly in that region. We also review the most recent laboratory experiments of reconnection driven by energetic laser beams, and discuss some important topics for future works.

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Section: Have Convincingly Showed That Both the Reconnection Sites Comentioning

confidence: 83%

Section: Have Convincingly Showed That Both the Reconnection Sites Comentioning

confidence: 99%

Section: The Reconnection Inflow Near the Current Sheetmentioning

confidence: 99%

Section: The Reconnection Inflow Near the Current Sheetmentioning

confidence: 99%

Section: The Reconnection Inflow Near the Current Sheetmentioning

confidence: 99%

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Review on Current Sheets in CME Development: Theories and Observations

et al. 2015

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Kinetic simulations of secondary reconnection in the reconnection jet

et al. 2015

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Magnetic reconnection, as one important energy dissipation process in plasmas, has been extensively studied in the past several decades. Magnetic reconnection occurring in the downstream of a primary X line is referred to as secondary reconnection. In this paper, we used kinetic simulations to investigate the secondary reconnection in detail. We found that secondary reconnection is reversed by the compression caused by the outflowing jet originating from the primary reconnection site, which results in the erosion of the magnetic island between the two X lines within~3 ω ci À1 . We show the observational signatures expected in electromagnetic fields and plasma measurements in the Earth's magnetotail, associated with this mechanism. These simulation results could be applied to interpret the signatures associated with the evolution of earthward magnetic islands in the Earth's magnetotail.

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Spontaneous reconnection at a separator current layer: 2. Nature of the waves and flows

Stevenson¹,

Parnell²

2015

JGR Space Physics

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Sudden destabilizations of the magnetic field, such as those caused by spontaneous reconnection, will produce waves and/or flows. Here we investigate the nature of the plasma motions resulting from spontaneous reconnection at a 3‐D separator. In order to clearly see these perturbations, we start from a magnetohydrostatic equilibrium containing two oppositely signed null points joined by a generic separator along which lies a twisted current layer. The nature of the magnetic reconnection initiated in this equilibrium as a result of an anomalous diffusivity is discussed in detail in Stevenson and Parnell (2015). The resulting sudden loss of force balance inevitably generates waves that propagate away from the diffusion region carrying the dissipated current. In their wake a twisting stagnation flow, in planes perpendicular to the separator, feeds flux back into the original diffusion site (the separator) in order to try to regain equilibrium. This flow drives a phase of slow weak impulsive bursty reconnection that follows on after the initial fast‐reconnection phase.

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Direct Observations of the Magnetic Reconnection Site of an Eruption on 2003 November 18

Cited by 305 publications

References 38 publications

Review on Current Sheets in CME Development: Theories and Observations

Review on Current Sheets in CME Development: Theories and Observations

Kinetic simulations of secondary reconnection in the reconnection jet

Spontaneous reconnection at a separator current layer: 2. Nature of the waves and flows

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