A Statistical Study of Main and Residual Accelerations of Coronal Mass Ejections

Zhang, J.

doi:10.1086/506903

Cited by 245 publications

(284 citation statements)

References 49 publications

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“…This is a strong acceleration but comparable to the average vertical rate of ∼4.5 km s −2 reported by Zhang & Dere (2006) for the X9.4 event on 1997 November 6. 17 This rate is also comparable to the 4.8 km s −2 rate (maintained for 2.7 minutes) assumed by Temmer et al (2009) to model the Moreton wave associated with an X3.8 flare on 2005 January 17.…”

Section: Kinematicssupporting

confidence: 82%

On the Origin of the Solar Moreton Wave of 2006 December 6

Balasubramaniam

Cliver

Pevtsov

et al. 2010

ApJ

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We analyzed ground-and space-based observations of the eruptive flare (3B/X6.5) and associated Moreton wave (∼850 km s −1 ; ∼270 • azimuthal span) of 2006 December 6 to determine the wave driver-either flare pressure pulse (blast) or coronal mass ejection (CME). Kinematic analysis favors a CME driver of the wave, despite key gaps in coronal data. The CME scenario has a less constrained/smoother velocity versus time profile than is the case for the flare hypothesis and requires an acceleration rate more in accord with observations. The CME picture is based, in part, on the assumption that a strong and impulsive magnetic field change observed by a GONG magnetograph during the rapid rise phase of the flare corresponds to the main acceleration phase of the CME. The Moreton wave evolution tracks the inferred eruption of an extended coronal arcade, overlying a region of weak magnetic field to the west of the principal flare in NOAA active region 10930. Observations of Hα foot point brightenings, disturbance contours in off-band Hα images, and He i 10830 Å flare ribbons trace the eruption from 18:42 to 18:44 UT as it progressed southwest along the arcade. Hinode EIS observations show strong blueshifts at foot points of this arcade during the post-eruption phase, indicating mass outflow. At 18:45 UT, the Moreton wave exhibited two separate arcs (one off each flank of the tip of the arcade) that merged and coalesced by 18:47 UT to form a single smooth wave front, having its maximum amplitude in the southwest direction. We suggest that the erupting arcade (i.e., CME) expanded laterally to drive a coronal shock responsible for the Moreton wave. We attribute a darkening in Hα from a region underlying the arcade to absorption by faint unresolved post-eruption loops.

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Section: Kinematicssupporting

confidence: 82%

On the Origin of the Solar Moreton Wave of 2006 December 6

Balasubramaniam

Cliver

Pevtsov

et al. 2010

ApJ

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“…This indicates that the two types of CMEs, the fast and slow ones, which were defined observationally [96,97], may be physically identical. This is consistent with recent statistical studies of CMEs based on a large sample of events [98][99][100]. Finally, the simulated eruption shown in Figure 8 is featured by the three-phase dynamical evolution including the initiation, main acceleration, and propagation phases agreeing with the observational finding of Zhang and Deer [100].…”

Section: Energy Release Mechanisms Of Cmes: Mhd Studies With a Flux-rsupporting

confidence: 91%

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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“…We reveal the evidence for the intrinsic helicity in the MFR: the observed helical threads winding around a possible common axis inside the MFR and the rotational motion of the filament materials along the two legs of the MFR descending into the chromosphere. Further kinematic analysis shows that the whole eruption process of the MFR, including the propagation in the outer corona, can be well characterized by three distinct kinematical evolution phases: the slow rise phase, the impulsive acceleration phase, and the deceleration phase, being similar to that of CMEs (Zhang et al 2001;Zhang & Dere 2006).…”

Section: Summary and Discussionmentioning

confidence: 90%

Tracking the Evolution of a Coherent Magnetic Flux Rope Continuously From the Inner to the Outer Corona

Cheng

Ding

Guo

et al. 2013

ApJ

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The magnetic flux rope (MFR) is believed to be the underlying magnetic structure of coronal mass ejections (CMEs). However, it remains unclear how an MFR evolves into and forms the multi-component structure of a CME. In this paper, we perform a comprehensive study of an extreme-ultraviolet (EUV) MFR eruption on 2013 May 22 by tracking its morphological evolution, studying its kinematics, and quantifying its thermal property. As EUV brightenings begin, the MFR starts to rise slowly and shows helical threads winding around an axis. Meanwhile, cool filamentary materials descend spirally down to the chromosphere. These features provide direct observational evidence of intrinsically helical structure of the MFR. Through detailed kinematical analysis, we find that the MFR evolution has two distinct phases: a slow rise phase and an impulsive acceleration phase. We attribute the first phase to the magnetic reconnection within the quasi-separatrix layers surrounding the MFR, and the much more energetic second phase to the fast magnetic reconnection underneath the MFR. We suggest that the transition between these two phases is caused by the torus instability. Moreover, we identify that the MFR evolves smoothly into the outer corona and appears as a coherent structure within the white-light CME volume. The MFR in the outer corona was enveloped by bright fronts that originated from plasma pile-up in front of the expanding MFR. The fronts are also associated with the preceding sheath region followed by the outmost MFR-driven shock.

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A Statistical Study of Main and Residual Accelerations of Coronal Mass Ejections

Cited by 245 publications

References 49 publications

On the Origin of the Solar Moreton Wave of 2006 December 6

On the Origin of the Solar Moreton Wave of 2006 December 6

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

Tracking the Evolution of a Coherent Magnetic Flux Rope Continuously From the Inner to the Outer Corona

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