Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/8338
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dc.contributor.authorMayank, Prateek-
dc.contributor.authorVaidya, Bhargav-
dc.contributor.authorMishra, Wageesh-
dc.contributor.authorChakrabarty, D-
dc.date.accessioned2024-01-25T05:47:46Z-
dc.date.available2024-01-25T05:47:46Z-
dc.date.issued2024-01-
dc.identifier.citationThe Astrophysical Journal Supplement Series, Vol. 270, No. 1, 10en_US
dc.identifier.issn0067-0049-
dc.identifier.urihttp://hdl.handle.net/2248/8338-
dc.descriptionOpen Accessen_US
dc.descriptionOriginal 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.abstractCoronal mass ejections (CMEs) are primary drivers of space weather, and studying their evolution in the inner heliosphere is vital to prepare for a timely response. Solar wind streams, acting as background, influence their propagation in the heliosphere and associated geomagnetic storm activity. This study introduces SWASTi-CME, a newly developed MHD-based CME model integrated into the Space Weather Adaptive SimulaTion (SWASTi) framework. It incorporates a nonmagnetized elliptic cone and a magnetized flux rope CME model. To validate the model’s performance with in situ observation at L1, two Carrington rotations were chosen: one during solar maxima with multiple CMEs, and one during solar minima with a single CME. The study also presents a quantitative analysis of CME–solar wind interaction using this model. To account for ambient solar wind effects, two scenarios of different complexity in solar wind conditions were established. The results indicate that ambient conditions can significantly impact some of the CME properties in the inner heliosphere. We found that the drag force on the CME front exhibits a variable nature, resulting in asymmetric deformation of the CME leading edge. Additionally, the study reveals that the impact on the distribution of CME internal pressure primarily occurs during the initial stage, while the CME density distribution is affected throughout its propagation. Moreover, regardless of the ambient conditions, it was observed that, after a certain propagation time (t), the CME volume follows a nonfractal power-law expansion (∝t 3.03−3.33) due to the attainment of a balanced state with ambient.en_US
dc.language.isoenen_US
dc.publisherAmerican Astronomical Societyen_US
dc.relation.urihttps://doi.org/10.3847/1538-4365/ad08c7-
dc.rights© 2023. The Author(s)-
dc.subjectSolar coronal mass ejections (310)en_US
dc.subjectSolar wind (1534)en_US
dc.subjectMagnetohydrodynamical simulations (1966)en_US
dc.titleSWASTi-CME: A Physics-based Model to Study Coronal Mass Ejection Evolution and Its Interaction with Solar Winden_US
dc.typeArticleen_US
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