Low-Frequency Type-II Radio Detections and Coronagraph Data Employed to Describe and Forecast the Propagation of 71 CMEs/Shocks

Cremades, H.; Iglesias, F. A.; Cyr, O. C. St.; Xie, H.; Kaiser, M. L.; Gopalswamy, Ν.

doi:10.1007/s11207-015-0776-y

Cited by 26 publications

(25 citation statements)

References 78 publications

(110 reference statements)

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“…Figure shows the average acceleration against the initial speed of the 71 CMEs included in the Cremades et al () study. The propagation profile of CME 3 (star symbol) lies at the edge of this distribution.…”

Section: Discussionmentioning

confidence: 99%

“…Type II radio burst emission can be used to track the CME-driven shock wave propagation through IP space. We follow the main methodology described in Cremades et al (2015) and focus our attention to the emission around and below 1 MHz to be consistent with their study. First, the type II radio emission is isolated from the rest of the spectra to avoid contamination by type III bursts.…”

Section: Ip Shock Propagation From Type II Radio Burstmentioning

confidence: 99%

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Modeling the Multiple CME Interaction Event on 6–9 September 2017 with WSA‐ENLIL+Cone

et al. 2019

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A series of coronal mass ejections (CMEs) erupted from the same active region between 4–6 September 2017. Later, on 6–9 September, two interplanetary (IP) shocks reached L1, creating a complex and geoeffective plasma structure. To understand the processes leading up to the formation of the two shocks, we model the CMEs with the Wang‐Sheeley‐Arge (WSA)‐ENLIL+Cone model. The first two CMEs merged already in the solar corona driving the first IP shock. In IP space, another fast CME presumably interacted with the flank of the preceding CMEs and caused the second shock detected in situ. By introducing a customized density enhancement factor (dcld) in the WSA‐ENLIL+Cone model based on coronagraph image observations, the predicted arrival time of the first IP shock was drastically improved. When the dcld factor was tested on a well‐defined single CME event from 12 July 2012 the shock arrival time saw similar improvement. These results suggest that the proposed approach may be an alternative to improve the forecast for fast and simple CMEs. Further, the slowly decelerating kilometric type II radio burst confirms that the properties of the background solar wind have been preconditioned by the passage of the first IP shock. This likely caused the last CME to experience insignificant deceleration and led to the early arrival of the second IP shock. This result emphasizes the need to take preconditioning of the IP medium into account when making forecasts of CMEs erupting in quick succession.

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Section: Discussionmentioning

confidence: 99%

Section: Ip Shock Propagation From Type II Radio Burstmentioning

confidence: 99%

Modeling the Multiple CME Interaction Event on 6–9 September 2017 with WSA‐ENLIL+Cone

et al. 2019

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“…The DT points derived from the low and white-light coronal data are fitted using d(t) = (at + b) + c, where the fit to the data is performed applying the same Levenberg-Marquardt least-square approximation as in Section 4.3. This equation was also applied by Cremades et al (2015) to fit points of a distance- time plot of a CME/shock that resulted from the combination of white-light corona, interplanetary type II radio, and in situ data. The fit is very good both in correspondence with the fast growth of the height in the low corona and also with the gradual increase registered later in the white-light corona.…”

Section: Correspondence Between Euv and White-light Featuresmentioning

confidence: 99%

Moreton and EUV Waves Associated with an X1.0 Flare and CME Ejection

et al. 2016

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Several other phenomena took place in connection with this event, such as low coronal waves and a coronal mass ejection (CME). We analyze the association between the Moreton wave and the EUV signatures observed with the Atmospheric Imaging Assembly onboard the Solar Dynamics Observatory. These include their low-coronal surface-imprint, and the signatures of the full wave and shock dome propagating outward in the corona. We also study their relation to the whitelight CME. We perform a kinematic analysis by tracking the wavefronts in several directions. This analysis reveals a high-directional dependence of accelerations and speeds determined from data at various wavelengths. We speculate that a region of open magnetic field lines northward of our defined radiant point sets favorable conditions for the propagation of a coronal magnetohydrodynamic shock in this direction. The hypothesis that the Moreton wavefront is produced by a coronal shock-wave that pushes the chromosphere downward is supported by the high compression ratio in that region. Furthermore, we propose a 3D geometrical model to explain the observed wavefronts as the chromospheric and low-coronal traces of an expanding and outward-traveling bubble intersecting the Sun. The results of the model are in agreement with the coronal shock-wave being generated by a 3D piston that expands at the speed of the associated rising filament. The piston is attributed to the fast ejection of the filament -CME ensemble, also consistent with the good match between the speed profiles of the low-coronal and white-light shock-waves.

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“…The GCS model can acquire the heliocentric distances of the CME leading front and has been successfully applied to SOHO and STEREO imaging observations (e.g., Thernisien et al 2009;Liu et al 2010;Cheng et al 2013;Mishra et al 2015). The frequency drift of type II radio bursts produced by CME-driven shocks can be converted to radial distances using a proper solar wind density model (e.g., Reiner et al 2007;Liu et al 2008Liu et al , 2013Cremades et al 2015;Hu et al 2016). Using the electron density model of Leblanc et al (1998, referred to as the Leblanc density model hereafter), Liu et al (2013) obtain the radial distances of CME-driven shocks from type II burst observations and find general consistency with those derived from triangulation techniques based on STEREO imaging observations.…”

Section: Introductionmentioning

confidence: 99%

Propagation Characteristics of Two Coronal Mass Ejections from the Sun Far into Interplanetary Space

Zhao

Liu

et al. 2017

ApJ

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Propagation of coronal mass ejections (CMEs) from the Sun far into interplanetary space is not well understood, due to limited observations. In this study we examine the propagation characteristics of two geo-effective CMEs, which occurred on 2005 May 6 and 13, respectively. Significant heliospheric consequences associated with the two CMEs are observed, including interplanetary CMEs (ICMEs) at the Earth and Ulysses, interplanetary shocks, a long-duration type II radio burst, and intense geomagnetic storms. We use coronagraph observations from SOHO/ LASCO, frequency drift of the long-duration type II burst, in situ measurements at the Earth and Ulysses, and magnetohydrodynamic propagation of the observed solar wind disturbances at 1 au to track the CMEs from the Sun far into interplanetary space. We find that both of the CMEs underwent a major deceleration within 1 au and thereafter a gradual deceleration when they propagated from the Earth to deep interplanetary space, due to interactions with the ambient solar wind. The results also reveal that the two CMEs interacted with each other in the distant interplanetary space even though their launch times on the Sun were well separated. The intense geomagnetic storm for each case was caused by the southward magnetic fields ahead of the CME, stressing the critical role of the sheath region in geomagnetic storm generation, although for the first case there is a corotating interaction region involved.

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Low-Frequency Type-II Radio Detections and Coronagraph Data Employed to Describe and Forecast the Propagation of 71 CMEs/Shocks

Cited by 26 publications

References 78 publications

Modeling the Multiple CME Interaction Event on 6–9 September 2017 with WSA‐ENLIL+Cone

Modeling the Multiple CME Interaction Event on 6–9 September 2017 with WSA‐ENLIL+Cone

Moreton and EUV Waves Associated with an X1.0 Flare and CME Ejection

Propagation Characteristics of Two Coronal Mass Ejections from the Sun Far into Interplanetary Space

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