Magnetohydrodynamic simulation of the interaction between interplanetary strong shock and magnetic cloud and its consequent geoeffectiveness: 2. Oblique collision

Xiong, Ming; Zheng, Huinan; Wang, Yuming; Wang, Shui

doi:10.1029/2006ja011901

Cited by 34 publications

(47 citation statements)

References 62 publications

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“…However, the presence of plasma material of CME1 trailing edge after the marked leading edge of CME2 cannot be denied, as the merging of both CMEs is in progress and continues beyond the Earth [ Liu et al , ]. The possibility of such mixing of CMEs have also been reported earlier which emphasize that signatures of CMEs interaction observed in situ depend on the relative orientation of the flux rope associated with both CMEs [ Xiong et al , , ; Lugaz et al , ; Lugaz and Farrugia , ].…”

Section: Resultsmentioning

confidence: 99%

Kinematics of interacting CMEs of 25 and 28 September 2012

2015

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We have studied two coronal mass ejections (CMEs) that occurred on 25 and 28 September 2012 and interacted near the Earth. By fitting the Graduated Cylindrical Shell model on the SECCHI/COR2 images and applying the Stereoscopic Self‐Similar Expansion method on the SECCHI/HI images, the initial direction of both the CMEs is estimated to be west of the Sun‐Earth line. Further, the three‐dimensional (3‐D) heliospheric kinematics of these CMEs have been estimated using Self‐Similar Expansion (SSE) reconstruction method. We show that the use of SSE method with different values of angular extent of the CMEs leads to significantly different kinematics estimates for the CMEs propagating away from the observer. Using the estimated kinematics and true masses of the CMEs, we have derived the coefficient of restitution for the collision which is found to be close to elastic. The in situ measurements at 1 AU show two distinct structures of interplanetary CMEs, heating of the following CME, and ongoing interaction between the preceding and the following CME. We highlight the signatures of interaction in remote and in situ observations of these CMEs and the role of interaction in producing a major geomagnetic storm.

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Section: Resultsmentioning

confidence: 99%

Kinematics of interacting CMEs of 25 and 28 September 2012

2015

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“…However, only few studies have been dedicated to understand the role of interacting CMEs in the generation of geomagnetic storms (Burlaga, Behannon, and Klein, 1987;Farrugia et al, 2006;Xiong et al, 2006). Our study is important as it focuses on the role of interacting CMEs in the generation of geomagnetic storms as well as substorms.…”

Section: Resultsmentioning

confidence: 99%

“…Thus, these interactions are of great importance from space weather point of view. Before the era of wide angle imaging far from the Sun, the understanding of involved physical mechanisms in CME-CME or CME-shock interaction was achieved mostly from magnetohydrodynamic (MHD) numerical simulations of the interaction of a shock wave with an magnetic cloud (MC) (Vandas et al, 1997;Vandas and Odstrcil, 2004;Xiong et al, 2006), the interaction of two ejecta (Gonzalez-Esparza, Santillán, and Ferrer, 2004;Lugaz, Manchester, and Gombosi, 2005;Wang et al, 2005), and the interaction of two MCs (Xiong et al, 2007;Xiong, Zheng, and Wang, 2009). have shown that a forward shock can cause an intense southward magnetic field of long duration in the preceding magnetic cloud.…”

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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“…A possible reason why the expansion rate is significantly below unity is that the MCs are perturbed by ambient solar wind and/or other transients as shown in observational statistics [ Gulisano et al , ], which may cause the external pressure surrounding the MC decreasing with distance more slowly than usual. The numerical simulations by, e.g., Xiong et al [, ], Lugaz et al [] also suggested that CME‐CME interaction may affect the expansion rate of the preceding CME.…”

Section: Statistical Properties Of Plasma Motionmentioning

confidence: 99%

Investigating plasma motion of magnetic clouds at 1 AU through a velocity‐modified cylindrical force‐free flux rope model

et al. 2015

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(2015), Investigating plasma motion of magnetic clouds at 1 AU through a velocity-modified cylindrical force-free flux rope model, J. Geophys. Res. Space Physics, 120, 1543-1565, doi:10.1002 and usually modeled by a flux rope. By assuming the quasi-steady evolution and self-similar expansion, we introduce three types of global motion into a cylindrical force-free flux rope model and developed a new velocity-modified model for MCs. The three types of the global motion are the linear propagating motion away from the Sun, the expanding, and the poloidal motion with respect to the axis of the MC. The model is applied to 72 MCs observed by Wind spacecraft to investigate the properties of the plasma motion of MCs. First, we find that some MCs had a significant propagation velocity perpendicular to the radial direction, suggesting the direct evidence of the CME's deflected propagation and/or rotation in interplanetary space. Second, we confirm the previous results that the expansion speed is correlated with the radial propagation speed and most MCs did not expand self-similarly at 1 AU. In our statistics, about 62%/17% of MCs underwent a underexpansion/overexpansion at 1 AU and the expansion rate is about 0.6 on average. Third, most interestingly, we find that a significant poloidal motion did exist in some MCs. Three speculations about the cause of the poloidal motion are therefore proposed. These findings advance our understanding of the MC's properties at 1 AU and the dynamic evolution of CMEs from the Sun to interplanetary space.

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Magnetohydrodynamic simulation of the interaction between interplanetary strong shock and magnetic cloud and its consequent geoeffectiveness: 2. Oblique collision

Cited by 34 publications

References 62 publications

Kinematics of interacting CMEs of 25 and 28 September 2012

Kinematics of interacting CMEs of 25 and 28 September 2012

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

Investigating plasma motion of magnetic clouds at 1 AU through a velocity‐modified cylindrical force‐free flux rope model

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