The CME-flare relationship: Are there really two types of CMEs?

Vršnak, Bojan; Sudar, D.; Ruždjak, Domagoj

doi:10.1051/0004-6361:20042166

Cited by 136 publications

(126 citation statements)

References 51 publications

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“…4 and 5), even the slowest events (V < 400 km s −1 ) are mostly decelerated (median acc = −2.5 m s −2 ). Such a behavior (except deceleration for the slowest events) was also observed in previous works (Yashiro et al 2004;Vršnak et al 2005). These events seem to be accelerated during the rising phase of flares and in the LASCO FOV the speed is determined by the drag force of the interplanetary medium.…”

Section: Summary and Discussionsupporting

confidence: 83%

“…The flare-associated CMEs are faster and decelerating, while the prominence-associated CMEs are slower and accelerating in the LASCO FOV (St. Cyr et al 1999). In a statistical analysis of 545 flare-associated CMEs and 104 non-flare CMEs, Vršnak et al (2005) found that both data sets have similar characteristics and form one consistent group of CMEs.…”

Section: Introductionmentioning

confidence: 98%

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Two types of flare-associated coronal mass ejections

Michałek¹

2008

A&A

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Aims. Here, we study the relationship between flares and CMEs. Methods. For this purpose a statistical analysis of 578 flare-associated CMEs is presented. We considered two types of flare-associated CMEs: CMEs that follow and precede flare onset. Results. We shown that both samples have quite different characteristics. The first type of CMEs tends to be decelerated (median acceleration = -5.0 m s −2 ), faster (median velocity = 519 km s −1 ), and physically related to flares (a correlation coefficient between the energy of the CME and the peak of the X-ray flare = 0.80). The CMEs preceding associated flares are mostly accelerated (median acceleration = 5.4 m s −2 ), slightly slower (median velocity = 487 km s −1 ), and poorly related to flares (a correlation coefficient between the energy of the CME and the peak of the X-ray flare = 0.12). Conclusions. These two types of flare-associated CMEs demonstrate that magnetic reconnection, which influences the CME acceleration, could be significantly different in the two types of events.

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Section: Summary and Discussionsupporting

confidence: 83%

Section: Introductionmentioning

confidence: 98%

Two types of flare-associated coronal mass ejections

Michałek¹

2008

A&A

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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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“…Statistical analysis by Yurchyshyn et al (2005) showed that the speed distribution for accelerating and decelerating events in the LASCO C2 and C3 fields of view are nearly identical and to a good approximation they can be fitting with a single lognormal distribution. Vršnak et al (2005) found that flare-associated CMEs and nonflare CMEs showed quite similar characteristics in the LASCO C2 and C3 fields of view, contradicting the concept of two types. We believe that the usage of the impulsive and gradual types should be limited to the convenience of reference.…”

Section: The Issue Of Cme Classificationmentioning

confidence: 69%

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

Zhang¹

2006

ApJ

241

230

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In this paper we present the results of a statistical study of the accelerations of coronal mass ejections (CMEs). A CME usually undergoes a multiphased kinematic evolution, with a main acceleration phase characterized by a rapid increase of CME velocity in the inner corona, followed by a relatively smooth propagation phase characterized by a constant speed or a small residual acceleration in the outer corona. We study both the main acceleration and the residual acceleration for 50 CME events based on Large Angle Spectrometric Coronagraph (LASCO) observations. We find that the magnitude of the main acceleration has a wide distribution, from 2.8 to 4464.0 m s À2 , with a median (average) value of 170.1 (330.9 m s À2 ), and a standard deviation of 644.8 m s À2 , whereas the magnitude of the residual acceleration ranges only from À131.0 to 52.0 m s À2 , with a median (average) value of 3.1 (0.9 m s À2 ) and a standard deviation of 25.3 m s À2 . The duration of the main acceleration is also widely distributed, from 6 to 1200 minutes, with a median (average) value of 54 (180 minutes) and a standard deviation of 286 minutes.We find an intriguing scaling law between the acceleration magnitude (A) and the acceleration duration (T ) over the entire parameter range of almost 3 orders of magnitude, which can be expressed as A (m s À2 ) ¼ 10; 000T À1 (minutes). The implications of these observational results on the issues of CME classification and CME modelings are discussed.

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The CME-flare relationship: Are there really two types of CMEs?

Cited by 136 publications

References 51 publications

Two types of flare-associated coronal mass ejections

Two types of flare-associated coronal mass ejections

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

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

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