Coronal and Interplanetary Propagation of CME/Shocks from Radio, In Situ and White‐Light Observations

Reiner, M. J.; Kaiser, M. L.; Bougeret, Jean‐Louis

doi:10.1086/518683

Cited by 84 publications

(128 citation statements)

References 54 publications

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“…Note that the density model describes the average radial variation of the density of the medium where the shock was propagating, so the scale factor n 0 is not necessarily the observed density at 1 AU. This analytical approach is different from previous studies which rely on a fit of the frequency drift of a type II burst (e.g., Reiner et al 2007;Liu et al 2008;Zhao et al 2017). It may set up a new paradigm in characterizing CME/shock propagation with long-duration type II bursts.…”

Section: Complex Type II Burst and Overall Propagation Profilementioning

confidence: 95%

“…The extent and cessation distance of the deceleration cannot be precisely determined given a single point of Doppler scintillation measurements in the former study and in the latter the large data gap between the Sun and 1 AU. Reiner et al (2007) argue that CME deceleration can cease anywhere from about 0.3 AU to beyond 1 AU based on a statistical analysis of interplanetary type II radio bursts, but their results indeed indicate that faster CMEs decelerate more rapidly and for shorter time periods. Using a triangulation technique based on the wide-angle heliospheric imaging observations from the twin STEREO spacecraft, Liu et al (2013) obtain the whole Sun-to-Earth propagation profile of fast CMEs, which typically shows three phases: an impulsive acceleration, then a rapid deceleration out to 40-80 solar radii, and finally a nearly constant speed or gradual deceleration.…”

Section: Introductionmentioning

confidence: 96%

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Propagation and Interaction Properties of Successive Coronal Mass Ejections in Relation to a Complex Type II Radio Burst

Liu

Zhao

Zhu

2017

ApJ

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We examine the propagation and interaction properties of three successive coronal mass ejections (CMEs) from 2001 November 21-22, with a focus on their connection with the behaviors of the associated long-duration complex type II radio burst. In combination with coronagraph and multi-point in situ observations, the long-duration type II burst provides key features for resolving the propagation and interaction complexities of the three CMEs. The two CMEs from November 22 interacted first and then overtook the November 21 CME at a distance of about 0.85 AU from the Sun. The time scale for the shock originally driven by the last CME to propagate through the preceding two CMEs is estimated to be about 14 and 6 hr, respectively. We present a simple analytical model without any free parameters to characterize the whole Sun-to-Earth propagation of the shock, which shows a remarkable consistency with all the available data and MHD simulations even out to the distance of Ulysses (2.34 AU). The coordination of in situ measurements at the Earth and Ulysses, which were separated by about 71.4• in latitude, gives important clues for the understanding of shock structure and the interpretation of in situ signatures. The results also indicate means to increase geo-effectiveness with multiple CMEs, which can be considered as another manifestation of the "perfect storm" scenario proposed by Liu et al. (2014a) although the current case is not "super" in the same sense as the 2012 July 23 event.

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Section: Complex Type II Burst and Overall Propagation Profilementioning

confidence: 95%

Section: Introductionmentioning

confidence: 96%

Propagation and Interaction Properties of Successive Coronal Mass Ejections in Relation to a Complex Type II Radio Burst

Liu

Zhao

Zhu

2017

ApJ

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“…There are different techniques that allow us to determine the distance at which the emission was produced relative to the observer. Some of these make use of electron density models, as demonstrated in the previous section, which provide a direct correlation between the observed frequency and the distance (height) at which they occur (e.g., Leblanc et al 1998;Reiner et al 2007). However, these techniques do not take into account inhomogeneities that may occur in both the interplanetary space and/or the ejected material.…”

Section: Direction-findingmentioning

confidence: 99%

The 2010 August 1 Type Ii Burst: A Cme-Cme Interaction and Its Radio and White-Light Manifestations

Oliveros

Raftery

Bain

et al. 2012

ApJ

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We present observational results of a type II burst associated with a CME -CME interaction observed in the radio and white-light wavelength range. We applied radio direction-finding techniques to observations from the STEREO and Wind spacecraft, the results of which were interpreted using white-light coronagraphic measurements for context. The results of the multiple radio-direction finding techniques applied were found to be consistent both with each other and with those derived from the white-light observations of coronal mass ejections (CMEs).The results suggest that the Type II burst radio emission is causally related to the CMEs interaction.

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“…The data points in Figure 7 are fitted with a simple kinematic model that was also used in Wood et al (2009aWood et al ( , 2009b, which assumes that the CME's motion can be represented by two phases of constant acceleration (or deceleration), a 1 and a 2 , which cease at times t 1 and t 2 , respectively, followed by a period of constant velocity. Reiner et al (2007) have used a similar kinematic model to reproduce the IPM propagation of CME shocks inferred from radio data. We use χ 2 minimization to zero on the best fit to the data (Bevington & Robinson 1992), where for this purpose we assume 1%, 2%, and 3% error bars for the COR1/COR2, HI1, and HI2 distance measurements, respectively, uncertainties that are educated estimates.…”

Section: Kinematic Modelmentioning

confidence: 99%

An Empirical Reconstruction of the 2008 April 26 Coronal Mass Ejection

Wood

Howard

2009

ApJ

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We present a three-dimensional model of the density distribution of a coronal mass ejection (CME) from 2008 April 26. This CME was observed by the two spacecraft composing the Solar Terrestrial Relations Observatory (STEREO), which tracked the CME from near the Sun, into the interplanetary medium (IPM), and all the way to 1 AU. The CME was directed toward STEREO-B and hit that spacecraft on 2008 April 29. The STEREO images of the CME show an internal structure that can be interpreted as having a flux rope shape. The two different perspectives on the event provided by the two STEREO spacecraft allow us to make a particularly strong argument for the flux rope interpretation, and the STEREO data also allow us to study the evolution of the flux rope in the IPM. The flux rope is oriented close to the ecliptic plane, but with the western leg tilted northwards by about 20 • . This implies an orientation roughly perpendicular to the neutral line of the active region at the event's point of origin, apparently an unusual geometry given that previous analyses have found that CME flux ropes are usually, but not always, oriented parallel to the neutral lines of their source regions. The CME model also consists of a front out ahead of the flux rope, possibly a shock launched by the flux rope driver. The model density distribution is reasonably successful at reproducing the CME appearance both close to the Sun in coronagraphic images, and far from the Sun in images of the IPM from STEREO's heliospheric imagers. This suggests that self-similar expansion is a reasonable first-order approximation for this particular CME, and also indicates that the flux rope's orientation does not change much during its journey through the IPM.

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Coronal and Interplanetary Propagation of CME/Shocks from Radio, In Situ and White‐Light Observations

Cited by 84 publications

References 54 publications

Propagation and Interaction Properties of Successive Coronal Mass Ejections in Relation to a Complex Type II Radio Burst

Propagation and Interaction Properties of Successive Coronal Mass Ejections in Relation to a Complex Type II Radio Burst

The 2010 August 1 Type Ii Burst: A Cme-Cme Interaction and Its Radio and White-Light Manifestations

An Empirical Reconstruction of the 2008 April 26 Coronal Mass Ejection

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