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Plunkett, S. P.; Vourlidas, A.; Šimberová, Stanislava; Karlický, M.; Kotrč, P.; Heinzel, P.; Kupryakov, Yu. A.; Guo, W. P.; Wu, S. T.

doi:10.1023/a:1005287524302

Cited by 118 publications

(67 citation statements)

References 28 publications

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“…This moderate acceleration continued until the CME reached a height of about 7.0 R . Events with similar intermediate kinematic characteristics have been reported before ( Plunkett et al 2000;Yurchyshyn 2002). The continuous distribution of CME kinematic properties is not consistent with the speculation that there may be two distinct classes of CMEs: impulsive CMEs and gradual CMEs Andrews & Howard 2001;Moon et al 2002;Zhang et al 2002).…”

Section: The Issue Of Cme Classificationsupporting

confidence: 74%

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

Zhang¹

2006

ApJ

246

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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Section: The Issue Of Cme Classificationsupporting

confidence: 74%

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

Zhang¹

2006

ApJ

246

230

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“…During its initial rise (until 13:30 UT) the prominence was seen to untwist, as in other events (cf. Kurokawa et al 1987;House & Berger 1987;Vršnak et al 1993;Plunkett et al 2000). Between 13:35 and 13:46 UT a bright blob detached from the leading edge of the rising prominence.…”

Section: Hα Observationsmentioning

confidence: 98%

The dynamics of an erupting prominence

Klein¹,

Mouradian²

2002

A&A

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Abstract. Hα full disk observations and radio interferometry at decimetre and metre wavelengths are used to probe the dynamics of ejecta and electron acceleration during a solar eruptive event on 1990 September 14. An erupting prominence and a moving type IV radio source are shown to trace a common magnetic structure during its rise from ∼10 Mm to 3 R above the limb. The height-time plot excludes a purely ballistic flight in the height range (0.5-3) R , but is consistent with both constant acceleration and constant velocity at heights ≥0.5 R . A plasma model of the radio emission is used to infer the mass and energetics of the ejected material. Electrons are accelerated in the surroundings of the rising structure, and in two flares up to 70 • away from the prominence. Radio observations provide evidence for large-scale interconnecting loops, but a physical connection between the eruption and the remote flares cannot be demonstrated.

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“…In recent years, a great deal of this speculation has centered on events that are described as having morphologies consistent with an underlying flux-rope geometry (Chen et al 1997;Dere et al 1999;Wood et al 1999;Wu et al 1999;Chen et al 2000;Plunkett et al 2000;Krall et al 2001;Chen & Krall 2003). Krall et al (2001) measured and modeled 11 such events, identifying them as ''flux-rope CMEs.''…”

Section: Introductionmentioning

confidence: 99%

Flux‐Rope Coronal Mass Ejection Geometry and Its Relation to Observed Morphology

Krall

Cyr

2006

ApJ

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A simple parameterization of a three-dimensional flux rope is used to determine a ''typical flux-rope geometry'' that corresponds to observed flux-rope coronal mass ejection (CME) morphologies (average apparent angular widths) at a leading-edge height of about 5.5 R . The parameterized flux rope, the curved axis of which is assumed to trace out an ellipse, is described in terms of the eccentricity of the ellipse, the width (minor diameter d ) of the flux rope at the apex, and the height of the apex above the solar surface 2R 1 . Assuming self-similar expansion, there are only two geometrical parameters to be determined: the eccentricity and the axial aspect ratio Ã a 2R 1 /d. For each pair of geometrical parameters, an ensemble of 72 orientations is considered, with each being specified in terms of a latitude angle, a longitude angle, and a rotation about the direction of motion. The resulting ensemble of synthetic coronagraph images is used to produce statistical measures of the morphology for comparison to corresponding observational measures from St. Cyr et al. (2004). We find that a typical flux-rope CME has ¼ 0:7 AE 0:2 and Ã a ¼ 1:1 AE 0:3. Subject headingg s: Sun: coronal mass ejections (CMEs)

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Cited by 118 publications

References 28 publications

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

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

The dynamics of an erupting prominence

Flux‐Rope Coronal Mass Ejection Geometry and Its Relation to Observed Morphology

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