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

Oliveros, J. C. Martinez; Raftery, C. L.; Bain, H. M.; Liu, Ying D.; Krupař, V.; Bale, S. D.; Krucker, S.

doi:10.1088/0004-637x/748/1/66

Cited by 65 publications

(44 citation statements)

References 38 publications

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“…We estimated the source location of the associated type II enhancement by applying radio DF and triangulation techniques to data from the Wind and STEREO radio instruments. Similar radio DF and triangulation methods were previously used to study the CME-CME interaction event on 2010 August 1 by Martínez Oliveros et al (2012b). They found evidence for a causal relationship between the type II radio burst and the CME-CME interaction.…”

Section: Introductionmentioning

confidence: 62%

Source Regions of the Type Ii Radio Burst Observed During a Cme–cme Interaction on 2013 May 22

Mäkelä

Gopalswamy

Reiner

et al. 2016

ApJ

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We report on our study of radio source regions during the type II radio burst on 2013 May 22 based on directionfinding analysis of the Wind/WAVES and STEREO/WAVES (SWAVES) radio observations at decameterhectometric wavelengths. The type II emission showed an enhancement that coincided with the interaction of two coronal mass ejections (CMEs) launched in sequence along closely spaced trajectories. The triangulation of the SWAVES source directions posited the ecliptic projections of the radio sources near the line connecting the Sun and the STEREO-A spacecraft. The WAVES and SWAVES source directions revealed shifts in the latitude of the radio source, indicating that the spatial location of the dominant source of the type II emission varies during the CME-CME interaction. The WAVES source directions close to 1 MHz frequencies matched the location of the leading edge of the primary CME seen in the images of the LASCO/C3 coronagraph. This correspondence of spatial locations at both wavelengths confirms that the CME-CME interaction region is the source of the type II enhancement. Comparison of radio and white-light observations also showed that at lower frequencies scattering significantly affects radio wave propagation.

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Section: Introductionmentioning

confidence: 62%

Source Regions of the Type Ii Radio Burst Observed During a Cme–cme Interaction on 2013 May 22

Mäkelä

Gopalswamy

Reiner

et al. 2016

ApJ

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“…Type II emissions are also used to study CME-CME interactions, a typical signature of which is an increase in the bandwidth and intensity of the type II burst (Gopalswamy et al 2001b). Martinez-Oliveros et al (2012) present an occasion of two interacting CMEs, where the type II burst appears to split into two bands with different drifting rates. Based on the study of the 2012 July 23 complex eruptions, Liu et al (2017) define a complex type II burst which is composed of multiple branches that may not all be fundamental-harmonic related.…”

Section: Introductionmentioning

confidence: 99%

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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“…As the current solar cycle progressed, interaction of CMEs now appears a fairly common phenomenon, in particular around solar maximum. The interacting CMEs of 2010 August 1 have been studied extensively by using primarily the STEREO white light imaging, near Earth in situ and, S-Waves radio observations Liu et al, 2012;Möstl et al, 2012;Temmer et al, 2012;Martínez Oliveros et al, 2012;Webb et al, 2013). Also, Lugaz et al (2012) have reported a clear deflection of 2010 May 23 -24 CMEs after their interaction.…”

Section: Introductionmentioning

confidence: 99%

“…(6) What are the favorable conditions for the CME's deflection and enhanced radio emission during CME-CME interaction? (Lugaz et al, 2012;Martínez Oliveros et al, 2012). In light of aforementioned questions and only a few studies reported, it is clear that the prediction of arrival time of interacting CMEs and association of remote observations of such CMEs with in situ is challenging.…”

Section: Introductionmentioning

confidence: 99%

Evolution and Consequences of Interacting CMEs of 9 – 10 November 2012 Using STEREO/SECCHI and In Situ Observations

2014

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Understanding of the kinematic evolution of Coronal Mass Ejections (CMEs) in the heliosphere is important to estimate their arrival time at the Earth. It is found that kinematics of CMEs can change when they interact or collide with each other as they propagate in the heliosphere. In this paper, we analyze the collision and post-interaction characteristics of two Earth-directed CMEs, launched successively on 2012 November 9 and 10, using white light imaging observations from STEREO/SECCHI and in situ observations taken from WIND spacecraft. We tracked two density enhanced features associated with leading and trailing edge of November 9 CME and one density enhanced feature associated with leading edge of November 10 CME by constructing J-maps. We found that the leading edge of November 10 CME interacted with the trailing edge of November 9 CME. We also estimated the kinematics of these features of the CMEs and found a significant change in their dynamics after interaction. In in situ observations, we identified distinct structures associated with interacted CMEs and also noticed their heating and compression as signatures of CME-CME interaction. Our analysis shows an improvement in arrival time prediction of CMEs using their post-collision dynamics than using pre-collision dynamics. Estimating the true masses and speeds of these colliding CMEs, we investigated the nature of observed collision which is found to be close to perfectly inelastic. The investigation also places in perspective the geomagnetic consequences of the two CMEs and their interaction in terms of occurrence of geomagnetic storm and triggering of magnetospheric substorms.

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

Cited by 65 publications

References 38 publications

Source Regions of the Type Ii Radio Burst Observed During a Cme–cme Interaction on 2013 May 22

Source Regions of the Type Ii Radio Burst Observed During a Cme–cme Interaction on 2013 May 22

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

Evolution and Consequences of Interacting CMEs of 9 – 10 November 2012 Using STEREO/SECCHI and In Situ Observations

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