A Study of the Kinematic Evolution of Coronal Mass Ejections

By J. Zhang, K. Dere, R. Howard, A. Vourlidas. 2004

239 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/3dcecb60510e9faf2557873d12bc135408dd0f01

How researchers see this paper

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In Astronomy and Astrophysics

1. M. Temmer
2. B. Vršnak
3. H. Hudson
4. R. Schwenn
5. Astrid Veronig
6. A. Vourlidas
7. S. Cranmer
8. J. C. Raymond

Citations in the corpus

• A Comparative Study between Eruptive X-Class Flares Associated with Coronal Mass Ejections and Confined X-Class Flares (2007, background): “In particular, Zhang et al. (2001) and Zhang et al. (2004) showed that the fast acceleration of CMEs in the inner corona coincides very well in time with the rise phase (or energy release phase) of the corresponding soft X-ray flares, strongly implying that both phenomena are driven by the same…”
• An Observational Overview of Solar Flares (2011, background): “Further studies revealed a close correlation between the CME acceleration and the derivative of the flare SXR flux, taken as a proxy for the flare enrgy release (Zhang et al. 2001, 2004; Maričić et al. 2007).”
• Acceleration in Fast Halo CMEs and Synchronized Flare HXR Bursts (2008, methodology): “From this raw distance-time measurements, , we derivedd(t) the CME plane-of-sky 1 velocity and acceleration pro-v(t) a(t) files by numerical derivative methods (analogous to the procedure used in Zhang et al. 2004).”
• COMBINED STEREO/RHESSI STUDY OF CORONAL MASS EJECTION ACCELERATION AND PARTICLE ACCELERATION IN SOLAR FLARES (2010, background): “Several authors found a correlation between the CME acceleration and the flare soft X-ray emission (Zhang et al. 2001, 2004; Zhang & Dere 2006; Vršnak et al. 2004; Maričić et al. 2007; Vršnak et al. 2007).”
• DIRECT EVIDENCE FOR A FAST CORONAL MASS EJECTION DRIVEN BY THE PRIOR FORMATION AND SUBSEQUENT DESTABILIZATION OF A MAGNETIC FLUX ROPE (2012, background): “The observed flare - flux rope dynamics largely conform with the well-known synchronization between flare emissions and CME acceleration (e.g., Zhang et al. 2001; Zhang et al. 2004; Maričić et al. 2007; Temmer et al. 2010; Bein et al. 2012).”
• Sixty-five years of solar radioastronomy: flares, coronal mass ejections and Sun–Earth connection (2008, background): “Zhang et al. (2004) concluded from this last association that the CME acceleration and the flare particle acceleration phases are strongly coupled.”
• Ultraviolet spectroscopy of the extended solar corona (2006, background): “This is the region where CMEs typically experience their maximum acceleration, acquiring most of their mass and kinetic energy (e.g., Zhang et al. 2004).”
• A Statistical Study of Main and Residual Accelerations of Coronal Mass Ejections (2006, background): “…CME events showed that a CME’s full kinematic evolution may un- dergo three distinct phases: (1) an ‘‘initiation phase’’ of slow rise, (2) an ‘‘acceleration phase’’ of rapid velocity increase, and (3) finally a ‘‘propagation phase’’ withminor velocity variation (Zhang et al. 2001, 2004).”
• The association of coronal mass ejections with their effects near the Earth (2005, background): “R. Schwenn et al.: The association of coronal mass ejections Zhang et al. (2001, 2004) described the initiation of CMEs in a three-phase scenario: the initiation phase, the impulsive acceleration phase and the propagation phase.”
• OBSERVING FLUX ROPE FORMATION DURING THE IMPULSIVE PHASE OF A SOLAR ERUPTION (2011, methodology): “From observations, Zhang et al. (2001, 2004) found that a flare-associated CME usually undergoes three distinct phases of evolution: the slow-rising initiation phase, the impulsive acceleration phase, and the near-constant propagation phase.”
• The CME-flare relationship: Are there really two types of CMEs? (2005, methodology): “For example, the two flare-CMEs studied by Zhang et al. (2004) attained the acceleration maximum at Article published by EDP Sciences and available at http://www.edpsciences.org/aa or http://dx.doi.org/10.1051/0004-6361:20042166 R ≈ 2 and R ≈ 5 solar radii.”