The launch of solar coronal mass ejections: Results from the coronal mass ejection onset program

Harrison, R. A.; Hildner, E.; Hundhausen, A. J.; Sime, D. G.; Simnett, G. M.

doi:10.1029/ja095ia02p00917

Cited by 108 publications

(50 citation statements)

References 30 publications

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“…The solar cycle variability of CME occurrence resembles the rate of increase of open solar flux at the source surface of potential coronal field models based on photospheric magnetograms ). These results complement what is known from the observations described above, especially in their suggestion that CMEs are linked to the evolution of the large scale coronal magnetic field (Harrison et al 1990). They also pave the way for STEREO investigations of the influence of active region emergence on CME genesis during the rise of cycle 24.…”

Section: Coronal Connectionssupporting

confidence: 73%

STEREO IMPACT Investigation Goals, Measurements, and Data Products Overview

et al. 2007

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The IMPACT (In situ Measurements of Particles And CME Transients) investigation on the STEREO mission was designed and developed to provide multipoint solar wind and suprathermal electron, interplanetary magnetic field, and solar energetic particle information required to unravel the nature of coronal mass ejections and their heliospheric consequences. IMPACT consists of seven individual sensors which are packaged into a boom suite, and a SEP suite. This review summarizes the science objectives of IMPACT, the instruments that comprise the IMPACT investigation, the accommodation of IMPACT on the STEREO twin spacecraft, and the overall data products that will flow from the IMPACT measurements. Accompanying papers in this volume of Space Science Reviews highlight the individual sensor technical details and capabilities, STEREO project plans for the use of IMPACT data, and modeling activities for IMPACT (and other STEREO) data interpretation.

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Section: Coronal Connectionssupporting

confidence: 73%

STEREO IMPACT Investigation Goals, Measurements, and Data Products Overview

et al. 2007

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“…The extrapolation method and its weakness were described in many literatures (e.g., Harrison & Sime 1989, Harrison et al 1990. We need to make at least two assumptions to obtain the extrapolated onsets.…”

Section: Temporal Relationshipmentioning

confidence: 99%

Statistical relationship between solar flares and coronal mass ejections

Yashiro

Gopalswamy

2008

Proc. IAU

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Abstract. We report on the statistical relationships between solar flares and coronal mass ejections (CMEs) observed during 1996-2007 inclusively. We used soft X-ray flares observed by the Geostationary Operational Environmental Satellite (GOES) and CMEs observed by the Large Angle and Spectrometric Coronagraph (LASCO) on board the Solar and Heliospheric Observatory (SOHO) mission. Main results are (1) the CME association rate increases with flare's peak flux, fluence, and duration, (2) the difference between flare and CME onsets shows a Gaussian distribution with the standard deviation σ = 17 min (σ = 15 min) for the first (second) order extrapolated CME onset, (3) the most frequent flare site is under the center of the CME span, not near one leg (outer edge) of the CMEs, (4) a good correlation was found between the flare fluence versus the CME kinetic energy. Implications for flare-CME models are discussed.

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“…The relative timing resembles the timeline of CME events derived from SMM observations (cf. Harrison et al 1990, and references therein): a "minor" soft X-ray event occurs at the rise of the mass ejection and is followed by a "major" event after the liftoff. We briefly present the observations and discuss the possibility of a physical link between the flares and the eruptive activity on the limb.…”

Section: Flaring Activity During the Eruptionmentioning

confidence: 99%

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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The launch of solar coronal mass ejections: Results from the coronal mass ejection onset program

Cited by 108 publications

References 30 publications

STEREO IMPACT Investigation Goals, Measurements, and Data Products Overview

STEREO IMPACT Investigation Goals, Measurements, and Data Products Overview

Statistical relationship between solar flares and coronal mass ejections

The dynamics of an erupting prominence

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