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Study of evolution and geo-effectiveness of coronal mass ejection–coronal mass ejection interactions using magnetohydrodynamic simulations with SWASTi framework

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dc.contributor.author Mayank, Prateek
dc.contributor.author Lotz, Stefan
dc.contributor.author Vaidya, Bhargav
dc.contributor.author Mishra, Wageesh
dc.contributor.author Chakrabarty, D
dc.date.accessioned 2024-12-05T05:48:31Z
dc.date.available 2024-12-05T05:48:31Z
dc.date.issued 2024-11-20
dc.identifier.citation The Astrophysical Journal, Vol 976, No.1, 126 en_US
dc.identifier.issn 1538-4357
dc.identifier.uri http://hdl.handle.net/2248/8596
dc.description Open Access en_US
dc.description Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI
dc.description.abstract The geo-effectiveness of coronal mass ejections (CMEs) is a critical area of study in space weather, particularly in the lesser-explored domain of CME–CME interactions and their geomagnetic consequences. This study leverages the Space Weather Adaptive SimulaTion framework to perform 3D MHD simulation of a range of CME–CME interaction scenarios within realistic solar wind conditions. The focus is on the dynamics of the initial magnetic flux, speed, density, and tilt of CMEs, and their individual and combined impacts on the disturbance storm time (Dst) index. Additionally, the kinematic, magnetic, and structural impacts on the leading CME, as well as the mixing of both CMEs, are analyzed. Time-series in situ studies are conducted through virtual spacecraft positioned along three different longitudes at 1 au. Our findings reveal that CME–CME interactions are nonuniform along different longitudes, due to the inhomogeneous ambient solar wind conditions. A significant increase in the momentum and kinetic energy of the leading CME is observed due to collisions with the trailing CME, along with the formation of reverse shocks in cases of strong interaction. These reverse shocks lead to complex wave patterns inside CME2, which can prolong the storm recovery phase. Furthermore, we observe that the minimum Dst value decreases with an increase in the initial density, tilt, and speed of the trailing CME. en_US
dc.language.iso en en_US
dc.publisher American Astronomical Society en_US
dc.relation.uri https://doi.org/10.3847/1538-4357/ad8084
dc.rights © 2024. The Author(s)
dc.subject Solar coronal mass ejections en_US
dc.subject Solar wind en_US
dc.subject Space weather en_US
dc.subject Interplanetary shocks en_US
dc.subject Magnetohydrodynamical simulations en_US
dc.subject Solar storm en_US
dc.title Study of evolution and geo-effectiveness of coronal mass ejection–coronal mass ejection interactions using magnetohydrodynamic simulations with SWASTi framework en_US
dc.type Article en_US


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