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Dere, K. P.; Brueckner, G. E.; Howard, R. A.; Koomen, M. J.; Korendyke, C. M.; Kreplin, R. W.; Michels, D. J.; Moses, J. D.; Moulton, N.; Socker, D. G.; Cyr, O. C. St.; Delaboudinière, J. P.; Artzner, G.; Brunaud, J.; Gabriel, A. H.; Hochedez, J.‐F.; Millier, F.; Song, Xueyan; Chauvineau, J.P.; Marioge, J P; Defise, Jean-Marc; Jamar, C.; Rochus, Pierre; Catura, R. C.; Lemen, J. R.; Gurman, J. B.; Neupert, W. M.; Clette, F.; Cugnon, P.; Dessel, E. L. van; Lamy, Philippe; Llebaria, A.; Schwenn, R.; Simnett, G. M.

doi:10.1023/a:1004907307376

Cited by 183 publications

(37 citation statements)

References 12 publications

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“…Figure 1(d ) shows that the bright CME legs matched well with the legs of the erupting prominence (indicated by the arrows), definitely indicating that the CME core was the erupting cool, dense prominence material in the outer corona. This is consistent with the results of Dere, et al (1997) and Plunkett, et al (2000). The CME front heights measured by Seiji Yashiro are shown in Figure 2(a), and the average velocity and acceleration from the first and second-order polynomial fits are 945 km s −1 and 24.7 m s −2 , respectively.…”

supporting

confidence: 90%

Eruption of a Large Quiescent Prominence and Associated CME on 2001 January 14

Jiang

et al. 2004

Proc. IAU

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Abstract. We present observations of a spectacular eruption of a huge quiescent prominence, which was clearly associated with a coronal mass ejection (CME). The CME consisted of a typical three-part structure: a bright loop-like leading edge, a dark cavity and a bright core. The prominence exhibited a very symmetrical loop-like eruption in low corona and matched well with the bright CME core trailing the CME leading edge. By combining the Hα, 17GHz and EUV observations with white-light coronagraphs observations, the bright CME core was conclusively identified as the erupting cool, dense prominence material.

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supporting

confidence: 90%

Eruption of a Large Quiescent Prominence and Associated CME on 2001 January 14

Jiang

et al. 2004

Proc. IAU

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“…Almost half of the CMEs, for example, originate on the far side of the Sun, for which no low-coronal observations had been available until the advent of STEREO. Nevertheless the X-ray observations of coronal dimmings and EUV observations of compact CME sources (Dere et al 1997a) had made it clear that there was often a very tight relationship between flares and CMEs. 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 energy release (Zhang et al 2001Maričić et al 2007).…”

Section: Flare Energy Release and Cme Dynamicsmentioning

confidence: 99%

An Observational Overview of Solar Flares

et al. 2011

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We present an overview of solar flares and associated phenomena, drawing upon a wide range of observational data primarily from the RHESSI era. Following an introductory discussion and overview of the status of observational capabilities, the article is split into topical sections which deal with different areas of flare phenomena (footpoints and ribbons, coronal sources, relationship to coronal mass ejections) and their interconnections. We also discuss flare soft X-ray spectroscopy and the energetics of the process. The emphasis is to describe the observations from multiple points of view, while bearing in mind the models that link them to each other and to theory. The present theoretical and observational understanding of solar flares is far from complete, so we conclude with a brief discussion of models, and a list of missing but important observations.

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“…Dere et al (1997) and Zhang et al (2001) presented early evidence for lateral expansion of CMEs in the low corona. The cartoon in Figure 17 shows the eruptive flare model (e.g., Figure 3 in Forbes 2000), with a Moreton wave added.…”

Section: Summary and Interpretationmentioning

confidence: 99%

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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Untitled

Cited by 183 publications

References 12 publications

Eruption of a Large Quiescent Prominence and Associated CME on 2001 January 14

Eruption of a Large Quiescent Prominence and Associated CME on 2001 January 14

An Observational Overview of Solar Flares

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

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