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

Savage, Sabrina; McKenzie, D. E.; Reeves, Katharine K.; Forbes, T. G.; Longcope, D. W.

doi:10.1088/0004-637x/722/1/329

Cited by 167 publications

(237 citation statements)

References 37 publications

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“…Savage et al (2010) noticed that the plasma flows were along a thin bright feature (see Fig. 13), which became more apparent after 11:00 UT and displaced 25 • southward within 6.5 hours at speed of about 4 • h −1 .…”

Section: Bi-directional Reconnection Outflows Observed In a Single Eventmentioning

confidence: 97%

“…Landi et al (2010) studied the initial acceleration phase of the CME in the same event, analyzed the physical properties of the CME core, and their data set included all other manifestations associated a CME: flare loops, CS, and coronal dimming. Landi et al (2012) extended the work of Landi et al (2010) to the diagnoses of plasma behind the CME, including that in the CS, to complement the works by Savage et al (2010) and Patsourakos and Vourlidas (2011) on the same event.…”

Section: Bi-directional Reconnection Outflows Observed In a Single Eventmentioning

confidence: 99%

“…To our knowledge, the eruptive event on April 9, 2008 is the first one in which both sunward and anti-sunward reconnection outflows were observed simultaneously (e.g., see Savage et al 2010). This event took place over the active region AR 10989, and produced an X-class flare and a CME.…”

Section: Bi-directional Reconnection Outflows Observed In a Single Eventmentioning

confidence: 99%

“…The change in the orientation of the current sheet resulted from the self-adjustment of the associated magnetic configuration in the eruption at speed of around 4 • h −1 . From Savage et al (2010) less bright structures above the active region to be recognized more easily. As the eruption was in progress, the CME moved away from the Sun like a cart wheel, so this CME is also known as the "cart-wheel CME".…”

Section: Bi-directional Reconnection Outflows Observed In a Single Eventmentioning

confidence: 99%

“…Focusing on the data from XRT and LASCO, and using the data from SECCHI for reference, Savage et al (2010) found a large amount of mass seen in EUV and SXR to be expelled from the Sun at speed ranging from 80 to 180 km s −1 in the time interval from 09:16 and 10:11 UT. Structures of the associated flare that could be seen were about 7 × 10 4 km above the limb.…”

Section: Bi-directional Reconnection Outflows Observed In a Single Eventmentioning

confidence: 99%

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Review on Current Sheets in CME Development: Theories and Observations

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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: Bi-directional Reconnection Outflows Observed In a Single Eventmentioning

confidence: 97%

Section: Bi-directional Reconnection Outflows Observed In a Single Eventmentioning

confidence: 99%

Section: Bi-directional Reconnection Outflows Observed In a Single Eventmentioning

confidence: 99%

Section: Bi-directional Reconnection Outflows Observed In a Single Eventmentioning

confidence: 99%

Section: Bi-directional Reconnection Outflows Observed In a Single Eventmentioning

confidence: 99%

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Review on Current Sheets in CME Development: Theories and Observations

et al. 2015

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Three‐dimensional outflow jets generated in collisionless magnetic reconnection

Fujimoto

2016

Geophysical Research Letters

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The present study proposes a new theoretical model generating three‐dimensional (3‐D) outflow jets in collisionless magnetic reconnection by means of a large‐scale particle‐in‐cell simulation. The key mechanism is the formation of 3‐D flux ropes arising in the turbulent electron current layer formed around the magnetic x line. The scale of the flux ropes along the current density is determined by the wavelength of an electron flow shear mode which is a macroscopic scale larger than the typical kinetic scales. The 3‐D flux ropes are intermittently ejected from the current layer and regulates the outflow jets into three dimensions. The gross reconnection rate is sufficiently large, since reconnection takes place almost uniformly along the x line.

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A model for stealth coronal mass ejections

Lynch

Masson

et al. 2016

JGR Space Physics

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Stealth coronal mass ejections (CMEs) are events in which there are almost no observable signatures of the CME eruption in the low corona but often a well‐resolved slow flux rope CME observed in the coronagraph data. We present results from a three‐dimensional numerical magnetohydrodynamics (MHD) simulation of the 1–2 June 2008 slow streamer blowout CME that Robbrecht et al. (2009) called “the CME from nowhere.” We model the global coronal structure using a 1.4 MK isothermal solar wind and a low‐order potential field source surface representation of the Carrington Rotation 2070 magnetogram synoptic map. The bipolar streamer belt arcade is energized by simple shearing flows applied in the vicinity of the helmet streamer's polarity inversion line. The flows are large scale and impart a shear typical of that expected from the differential rotation. The slow expansion of the energized helmet streamer arcade results in the formation of a radial current sheet. The subsequent onset of expansion‐induced flare reconnection initiates the stealth CME while gradually releasing the stored magnetic energy. We present favorable comparisons between our simulation results and the multiviewpoint SOHO‐LASCO (Large Angle and Spectrometric Coronagraph) and STEREO‐SECCHI (Sun Earth Connection Coronal and Heliospheric Investigation) coronagraph observations of the preeruption streamer structure and the initiation and evolution of the stealth streamer blowout CME.

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

Cited by 167 publications

References 37 publications

Review on Current Sheets in CME Development: Theories and Observations

Review on Current Sheets in CME Development: Theories and Observations

Three‐dimensional outflow jets generated in collisionless magnetic reconnection

A model for stealth coronal mass ejections

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