A Statistical Study on the Morphology of Rays and Dynamics of Blobs in the Wake of Coronal Mass Ejections

Song, Hongqiang; Kong, Xiangliang; Chen, Yao; Li, Bo; Li, Gang; Feng, Shiwei; Xia, Lidong

doi:10.1007/s11207-011-9848-9

Cited by 34 publications

(28 citation statements)

References 31 publications

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“…So for the time being, studying the brightness distribution is the only approach via which more or less, we are able to look into the geometric structure and physical properties of the CS. In addition to the thermal halo, it is possible that, like the case of the helmet streamer, the CME/flare CS itself is actually very thin and embedded in a thick plasma sheet that could be recognized according to the brightness, and the CS thickness is actually much smaller than that of the plasma sheet (e.g., see also Song et al 2012).…”

Section: Discussionmentioning

confidence: 99%

“…After having analyzed the LASCO data obtained in the time interval between 1996 and 2009, Song et al (2012) found more plasma blobs flowing inside the post-CME CS. The speeds of these blobs spread over the range from 200 to 10 3 km s −1 .…”

Section: Upward Reconnection Outflowsmentioning

confidence: 99%

“…These results are consistent with those of Ko et al (2003) and Lin et al (2005), and suggest a positive correlation of the outflow speed with the class of the associated flare. In addition, Song et al (2012) also studied the plasma blobs flowing inside the helmet streamer, and noticed that these blobs are apparently slower than those inside the CME current sheet. They concluded that the difference in velocities of plasma blobs could be ascribed to the reconnection processes occurring in the different environments.…”

Section: Upward Reconnection Outflowsmentioning

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: Discussionmentioning

confidence: 99%

Section: Upward Reconnection Outflowsmentioning

confidence: 99%

Section: Upward Reconnection Outflowsmentioning

confidence: 99%

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Review on Current Sheets in CME Development: Theories and Observations

et al. 2015

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“…Song et al [62] conducted a survey through the LASCO data obtained in 2007 and did find 10 multi-blob events with 106 blobs in total. All events last for 3-4 d. In Figure 5 velocity profiles for all blobs observed in Song et al [70] are plotted together. From this figure and other plots not shown here, it can be seen that all velocities increase monotonically with radial distance, and vary in a relatively small range of < 300 km s 1 .…”

Section: Persistent Releases Of Streamer Blobs and Diagnostics Of Neamentioning

confidence: 96%

“…Velocity-distance (in units of solar radii) profiles for the 45 post-CME blobs collected by Song et al [70] (black circles) and the 106 streamer blobs (red pluses) given by Song et al [62]. A blue line is drawn to separate their velocity distributions, which is given by the average of the polynomial fittings to the two groups of velocity measurements and expressed as v=0.1r 2 +13.7r+246 with v and r in units of km s 1 and Rs, respectively.…”

Section: Figurementioning

confidence: 99%

A review of recent studies on coronal dynamics: Streamers, coronal mass ejections, and their interactions

Chen

2013

Chin. Sci. Bull.

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In this article I present a review of recent studies on coronal dynamics, including research progresses on the physics of coronal streamers that are the largest structure in the corona, physics of coronal mass ejections (CMEs) that may cause a global disturbance to the corona, as well as physics of CME-streamer interactions. The following topics will be discussed in depth: (1) acceleration of the slow wind flowing around the streamer considering the effect of magnetic flux tube curvature; (2) physical mechanism accounting for persistent releases of streamer blobs and diagnostic results on the temporal variability of the slow wind speed with such events; (3) force balance analysis and energy release mechanism of CMEs with a flux rope magnetohydrodynamic model; (4) statistical studies on magnetic islands along the coronal-ray structure behind a CME and the first observation of magnetic island coalescence with associated electron acceleration; and (5) white light and radio manifestations of CME-streamer interactions. These studies shed new light on the physics of coronal streamers, the acceleration of the slow wind, the physics of solar eruptions, the physics of magnetic reconnection and associated electron acceleration, the large-scale coronal wave phenomenon, as well as the physics accounting for CME shock-induced type II radio bursts. solar wind, coronal streamer, coronal mass ejection, solar radio burst, magnetic reconnection Citation:Chen Y. A review of recent studies on coronal dynamics: Streamers, coronal mass ejections, and their interactions.

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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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A Statistical Study on the Morphology of Rays and Dynamics of Blobs in the Wake of Coronal Mass Ejections

Cited by 34 publications

References 31 publications

Review on Current Sheets in CME Development: Theories and Observations

Review on Current Sheets in CME Development: Theories and Observations

A review of recent studies on coronal dynamics: Streamers, coronal mass ejections, and their interactions

A model for stealth coronal mass ejections

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