Magnetohydrodynamic simulation of the interaction between two interplanetary magnetic clouds and its consequent geoeffectiveness: 2. Oblique collision

Abstract

The numerical studies of the interplanetary coupling between multiple magnetic clouds (MCs) are continued by a 2.5-dimensional ideal magnetohydrodynamic (MHD) model in the heliospheric meridional plane. The interplanetary direct collision (DC) / oblique collision (OC) between both MCs results from their same/different initial propagation orientations. Here the OC is explored in contrast to the results of the DC (Xiong et al., 2007). Both the slow MC1 and fast MC2 are consequently injected from the different heliospheric latitudes to form a compound stream during the interplanetary propagation. The MC1 and MC2 undergo contrary deflections during the process of oblique collision. Their deflection angles of $|\delta {\theta }_1|$ and $|\delta {\theta }_2|$ continuously increase until both MC-driven shock fronts are merged into a stronger compound one. The $|\delta {\theta }_1|$, $|\delta {\theta }_2|$, and total deflection angle $\Delta \theta$ ($\Delta \theta =|\delta {\theta }_1|+|\delta {\theta }_2|$) reach their corresponding maxima when the initial eruptions of both MCs are at an appropriate angular difference. Moreover, with the increase of MC2's initial speed, the OC becomes more intense, and the enhancement of $\delta {\theta }_1$ is much more sensitive to $\delta {\theta }_2$. The $|\delta {\theta }_1|$ is generally far less than the $|\delta {\theta }_2|$, and the unusual case of $|\delta {\theta }_1|\simeq |\delta {\theta }_2|$ only occurs for an extremely violent OC. But because of the elasticity of the MC body to buffer the collision, this deflection would gradually approach an asymptotic degree. Therefore, the deflection due to the OC should be considered for the evolution and ensuing geoeffectiveness of interplanetary interaction among successive coronal mass ejections (CMEs).

51 pages, 13 figures, JGR - Space Physics, in press

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• Statistical Study of Coronal Mass Ejection Source Locations: Understanding CMEs Viewed in Coronagraphs
• The Interaction of Two Coronal Mass Ejections: Influence of Relative Orientation
• Dynamical evolution of a magnetic cloud from the Sun to 5.4 AU
• The Heliocentric Distance Where the Deflections and Rotations of Solar Coronal Mass Ejections Occur
• Full Halo Coronal Mass Ejections: Arrival at the Earth
• Signatures of magnetic reconnection at boundaries of interplanetary small-scale magnetic flux ropes
• Kinematics of Interacting CMEs of September 25 and 28, 2012
• Assessing the collision nature of coronal mass ejections in the inner heliosphere
• On Understanding the Nature of Collision of Coronal Mass Ejections Observed by \textit{STEREO}
• Propagation of Coronal Mass Ejections from the Sun to Earth
• Using Coordinated Observations in Polarised White Light and Faraday Rotation to Probe the Spatial Position and Magnetic Field of an Interplanetary Sheath
• Forward modelling to determine the observational signatures of white-light imaging and interplanetary scintillation for the propagation of an interplanetary shock in the ecliptic plane