Application of a Modified Spheromak Model to Simulations of Coronal Mass Ejection in the Inner Heliosphere
Abstract The magnetic fields of interplanetary coronal mass ejections (ICMEs), which originate close to the Sun in the form of a flux rope, determine their geoeffectiveness. Therefore, robust flux rope‐based models of CMEs are required to perform magnetohydrodynamic (MHD) simulations aimed at space...
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| Format: | Article |
| Language: | English |
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Wiley
2020-05-01
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| Series: | Space Weather |
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| Online Access: | https://doi.org/10.1029/2019SW002405 |
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| author | Talwinder Singh Tae K. Kim Nikolai V. Pogorelov Charles N. Arge |
| author_facet | Talwinder Singh Tae K. Kim Nikolai V. Pogorelov Charles N. Arge |
| author_sort | Talwinder Singh |
| collection | DOAJ |
| description | Abstract The magnetic fields of interplanetary coronal mass ejections (ICMEs), which originate close to the Sun in the form of a flux rope, determine their geoeffectiveness. Therefore, robust flux rope‐based models of CMEs are required to perform magnetohydrodynamic (MHD) simulations aimed at space weather predictions. We propose a modified spheromak model and demonstrate its applicability to CME simulations. In this model, such properties of a simulated CME as the poloidal and toroidal magnetic fluxes, and the helicity sign can be controlled with a set of input parameters. We propose a robust technique for introducing CMEs with an appropriate speed into a background, MHD solution describing the solar wind in the inner heliosphere. Through a parametric study, we find that the speed of a CME is much more dependent on its poloidal flux than on the toroidal flux. We also show that the CME speed increases with its total energy, giving us control over its initial speed. We further demonstrate the applicability of this model to simulations of CME‐CME collisions. Finally, we use this model to simulate the 12 July 2012 CME and compare the plasma properties at 1 AU with observations. The predicted CME properties agree reasonably with observational data. |
| format | Article |
| id | doaj-art-f87f3a4d191e4ee198c0d437b6567f9a |
| institution | Kabale University |
| issn | 1542-7390 |
| language | English |
| publishDate | 2020-05-01 |
| publisher | Wiley |
| record_format | Article |
| series | Space Weather |
| spelling | doaj-art-f87f3a4d191e4ee198c0d437b6567f9a2025-01-14T16:27:36ZengWileySpace Weather1542-73902020-05-01185n/an/a10.1029/2019SW002405Application of a Modified Spheromak Model to Simulations of Coronal Mass Ejection in the Inner HeliosphereTalwinder Singh0Tae K. Kim1Nikolai V. Pogorelov2Charles N. Arge3Department of Space Science The University of Alabama in Huntsville Huntsville AL USACenter for Space Plasma and Aeronomic Research The University of Alabama in Huntsville Huntsville AL USADepartment of Space Science The University of Alabama in Huntsville Huntsville AL USASolar Physics Laboratory NASA/GSFC Greenbelt MD USAAbstract The magnetic fields of interplanetary coronal mass ejections (ICMEs), which originate close to the Sun in the form of a flux rope, determine their geoeffectiveness. Therefore, robust flux rope‐based models of CMEs are required to perform magnetohydrodynamic (MHD) simulations aimed at space weather predictions. We propose a modified spheromak model and demonstrate its applicability to CME simulations. In this model, such properties of a simulated CME as the poloidal and toroidal magnetic fluxes, and the helicity sign can be controlled with a set of input parameters. We propose a robust technique for introducing CMEs with an appropriate speed into a background, MHD solution describing the solar wind in the inner heliosphere. Through a parametric study, we find that the speed of a CME is much more dependent on its poloidal flux than on the toroidal flux. We also show that the CME speed increases with its total energy, giving us control over its initial speed. We further demonstrate the applicability of this model to simulations of CME‐CME collisions. Finally, we use this model to simulate the 12 July 2012 CME and compare the plasma properties at 1 AU with observations. The predicted CME properties agree reasonably with observational data.https://doi.org/10.1029/2019SW002405MHDcoronal mass ejectionssolar windspace weatherpredictionflux ropes |
| spellingShingle | Talwinder Singh Tae K. Kim Nikolai V. Pogorelov Charles N. Arge Application of a Modified Spheromak Model to Simulations of Coronal Mass Ejection in the Inner Heliosphere Space Weather MHD coronal mass ejections solar wind space weather prediction flux ropes |
| title | Application of a Modified Spheromak Model to Simulations of Coronal Mass Ejection in the Inner Heliosphere |
| title_full | Application of a Modified Spheromak Model to Simulations of Coronal Mass Ejection in the Inner Heliosphere |
| title_fullStr | Application of a Modified Spheromak Model to Simulations of Coronal Mass Ejection in the Inner Heliosphere |
| title_full_unstemmed | Application of a Modified Spheromak Model to Simulations of Coronal Mass Ejection in the Inner Heliosphere |
| title_short | Application of a Modified Spheromak Model to Simulations of Coronal Mass Ejection in the Inner Heliosphere |
| title_sort | application of a modified spheromak model to simulations of coronal mass ejection in the inner heliosphere |
| topic | MHD coronal mass ejections solar wind space weather prediction flux ropes |
| url | https://doi.org/10.1029/2019SW002405 |
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