High-resolution Simulation of Coronal Mass Ejection–Corotating Interaction Region Interactions: Mesoscale Solar Wind Structure Formation Observable by the SWIFT Constellation Article Swipe
W. B. Manchester
,
Nishtha Sachdeva
,
Emilia Kilpua
,
Matti Ala‐Lahti
,
Shirsh Lata Soni
,
Zhenguang Huang
,
Hongfan Chen
,
Aniket Jivani
,
B. van der Holst
,
Á. Szabó
,
Mojtaba Akhavan‐Tafti
·
YOU?
·
· 2025
· Open Access
·
· DOI: https://doi.org/10.3847/1538-4357/adf855
YOU?
·
· 2025
· Open Access
·
· DOI: https://doi.org/10.3847/1538-4357/adf855
We present an unprecedented simulation of how two large-scale heliospheric transients—a coronal mass ejection (CME) and a corotating stream interaction region—collide, producing a dramatic increase in the complexity of the CME due to formation of mesoscale flux ropes. These structures are captured for the first time by a numerical simulation using high-resolution numerical grids. The circumstances that lead to the formation of these complex structures occur during solar maximum. At the time of the solar maximum taken for this study, 2014 September, the heliospheric current sheet is vertically inclined running over the poles, allowing the CME to impact a preceding slow-fast stream interaction region. The simulation is performed with the Alfvén Wave Solar Atmosphere Model (or AWSoM), with which we initiate a fast CME from active region (AR) 12158 by applying a Gibson–Low magnetic flux rope. Magnetic reconnection within the leading extremity of the CME results in the formation of mesoscale flux ropes, which contain sufficiently strong magnetic fields (∼30 nT) to affect planetary magnetospheres. Finally, we use a tetrahedral configuration of four virtual probes, corresponding to the Space Weather Investigation Frontier mission concept, to show that the mission can uniquely resolve the spatial characteristics and temporal evolution of reconnecting current sheets within the CME, as well as the resulting mesoscale structures.
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- Type
- article
- Language
- en
- Landing Page
- https://doi.org/10.3847/1538-4357/adf855
- OA Status
- gold
- Cited By
- 1
- References
- 90
- OpenAlex ID
- https://openalex.org/W4414872862
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https://openalex.org/W4414872862Canonical identifier for this work in OpenAlex
- DOI
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https://doi.org/10.3847/1538-4357/adf855Digital Object Identifier
- Title
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High-resolution Simulation of Coronal Mass Ejection–Corotating Interaction Region Interactions: Mesoscale Solar Wind Structure Formation Observable by the SWIFT ConstellationWork title
- Type
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articleOpenAlex work type
- Language
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enPrimary language
- Publication year
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2025Year of publication
- Publication date
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2025-10-06Full publication date if available
- Authors
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W. B. Manchester, Nishtha Sachdeva, Emilia Kilpua, Matti Ala‐Lahti, Shirsh Lata Soni, Zhenguang Huang, Hongfan Chen, Aniket Jivani, B. van der Holst, Á. Szabó, Mojtaba Akhavan‐TaftiList of authors in order
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https://doi.org/10.3847/1538-4357/adf855Publisher landing page
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YesWhether a free full text is available
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goldOpen access status per OpenAlex
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https://doi.org/10.3847/1538-4357/adf855Direct OA link when available
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1Total citation count in OpenAlex
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2025: 1Per-year citation counts (last 5 years)
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90Number of works referenced by this work
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| abstract_inverted_index.virtual | 174 |
| abstract_inverted_index.Abstract | 0 |
| abstract_inverted_index.Finally, | 166 |
| abstract_inverted_index.Frontier | 182 |
| abstract_inverted_index.Magnetic | 137 |
| abstract_inverted_index.allowing | 94 |
| abstract_inverted_index.applying | 131 |
| abstract_inverted_index.captured | 42 |
| abstract_inverted_index.concept, | 184 |
| abstract_inverted_index.dramatic | 24 |
| abstract_inverted_index.ejection | 14 |
| abstract_inverted_index.inclined | 89 |
| abstract_inverted_index.increase | 25 |
| abstract_inverted_index.initiate | 121 |
| abstract_inverted_index.magnetic | 134, 158 |
| abstract_inverted_index.maximum. | 69 |
| abstract_inverted_index.temporal | 197 |
| abstract_inverted_index.uniquely | 191 |
| abstract_inverted_index.evolution | 198 |
| abstract_inverted_index.extremity | 142 |
| abstract_inverted_index.formation | 34, 61, 149 |
| abstract_inverted_index.mesoscale | 36, 151, 211 |
| abstract_inverted_index.numerical | 49, 53 |
| abstract_inverted_index.performed | 108 |
| abstract_inverted_index.planetary | 164 |
| abstract_inverted_index.preceding | 100 |
| abstract_inverted_index.producing | 22 |
| abstract_inverted_index.resulting | 210 |
| abstract_inverted_index.slow-fast | 101 |
| abstract_inverted_index.Atmosphere | 114 |
| abstract_inverted_index.September, | 82 |
| abstract_inverted_index.complexity | 28 |
| abstract_inverted_index.corotating | 18 |
| abstract_inverted_index.simulation | 5, 50, 106 |
| abstract_inverted_index.structures | 40, 65 |
| abstract_inverted_index.vertically | 88 |
| abstract_inverted_index.interaction | 20, 103 |
| abstract_inverted_index.large-scale | 9 |
| abstract_inverted_index.structures. | 212 |
| abstract_inverted_index.tetrahedral | 170 |
| abstract_inverted_index.Gibson–Low | 133 |
| abstract_inverted_index.heliospheric | 10, 84 |
| abstract_inverted_index.reconnecting | 200 |
| abstract_inverted_index.reconnection | 138 |
| abstract_inverted_index.sufficiently | 156 |
| abstract_inverted_index.Investigation | 181 |
| abstract_inverted_index.circumstances | 56 |
| abstract_inverted_index.configuration | 171 |
| abstract_inverted_index.corresponding | 176 |
| abstract_inverted_index.unprecedented | 4 |
| abstract_inverted_index.transients—a | 11 |
| abstract_inverted_index.characteristics | 195 |
| abstract_inverted_index.high-resolution | 52 |
| abstract_inverted_index.magnetospheres. | 165 |
| abstract_inverted_index.region—collide, | 21 |
| cited_by_percentile_year.max | 95 |
| cited_by_percentile_year.min | 91 |
| countries_distinct_count | 0 |
| institutions_distinct_count | 11 |
| citation_normalized_percentile.value | 0.89510146 |
| citation_normalized_percentile.is_in_top_1_percent | False |
| citation_normalized_percentile.is_in_top_10_percent | True |