Influence of an Upstream Dynamic Pressure Pulse on Venus–Solar Wind Interaction by Multispecies Magnetohydrodynamic Simulation
As an unmagnetized planet, Venus does not have a global dipole magnetic field like Earth. The solar wind interacts directly with the Venusian ionosphere. In this paper, the interaction between solar wind and the Venusian upper atmosphere is investigated by conducting a three-dimensional multispecies...
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IOP Publishing
2023-01-01
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Series: | The Astrophysical Journal |
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Online Access: | https://doi.org/10.3847/1538-4357/acfca7 |
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author | Yun Li Ruijing Xiong Haoyu Lu Jinbin Cao Tianle Zhu Guokan Li Shibang Li |
author_facet | Yun Li Ruijing Xiong Haoyu Lu Jinbin Cao Tianle Zhu Guokan Li Shibang Li |
author_sort | Yun Li |
collection | DOAJ |
description | As an unmagnetized planet, Venus does not have a global dipole magnetic field like Earth. The solar wind interacts directly with the Venusian ionosphere. In this paper, the interaction between solar wind and the Venusian upper atmosphere is investigated by conducting a three-dimensional multispecies magnetohydrodynamic (MHD) model, in which the Venusian ionosphere is developed self-consistently by considering chemical reactions among four major ion species (H ^+ , O _2 ^+ , O ^+ , and CO _2 ^+ ). Based on this developed MHD model, we mainly study the effects of the impulsive solar wind dynamic pressure on the interaction process. Simulation results reveal that the locations of the bow shock and magnetic pileup boundary show an abrupt compression, then expansion, and finally shrinkage to reach a new steady state with the influence of the impulsive dynamic pressure. The recovery time of the large-scale magnetic field is a few minutes. In addition, the peak escape fluxes are enhanced by about 1 order of magnitude due to the increased solar wind dynamic pressure pulse. |
first_indexed | 2024-03-10T16:49:59Z |
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language | English |
last_indexed | 2024-03-10T16:49:59Z |
publishDate | 2023-01-01 |
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spelling | doaj.art-9a497006d40b4013be9ad7eb5fe283002023-11-20T11:20:02ZengIOP PublishingThe Astrophysical Journal1538-43572023-01-01958214210.3847/1538-4357/acfca7Influence of an Upstream Dynamic Pressure Pulse on Venus–Solar Wind Interaction by Multispecies Magnetohydrodynamic SimulationYun Li0https://orcid.org/0000-0001-8953-7936Ruijing Xiong1Haoyu Lu2Jinbin Cao3Tianle Zhu4Guokan Li5https://orcid.org/0000-0003-2161-8339Shibang Li6https://orcid.org/0000-0001-9175-0007School of Space and Environment, Beihang University , Beijing 100191, People’s Republic of China ; lvhy@buaa.edu.cn; Key Laboratory of Space Environment Monitoring and Information Processing, Ministry of Industry and Information Technology , Beijing 100191, People’s Republic of China; State Key Laboratory of Lunar and Planetary Sciences, Macau University of Science and Technology , Taipa 999078, Macau, People’s Republic of ChinaSchool of Space and Environment, Beihang University , Beijing 100191, People’s Republic of China ; lvhy@buaa.edu.cnSchool of Space and Environment, Beihang University , Beijing 100191, People’s Republic of China ; lvhy@buaa.edu.cn; Key Laboratory of Space Environment Monitoring and Information Processing, Ministry of Industry and Information Technology , Beijing 100191, People’s Republic of ChinaSchool of Space and Environment, Beihang University , Beijing 100191, People’s Republic of China ; lvhy@buaa.edu.cn; Key Laboratory of Space Environment Monitoring and Information Processing, Ministry of Industry and Information Technology , Beijing 100191, People’s Republic of ChinaSchool of Space and Environment, Beihang University , Beijing 100191, People’s Republic of China ; lvhy@buaa.edu.cnSchool of Space and Environment, Beihang University , Beijing 100191, People’s Republic of China ; lvhy@buaa.edu.cnSchool of Space and Environment, Beihang University , Beijing 100191, People’s Republic of China ; lvhy@buaa.edu.cnAs an unmagnetized planet, Venus does not have a global dipole magnetic field like Earth. The solar wind interacts directly with the Venusian ionosphere. In this paper, the interaction between solar wind and the Venusian upper atmosphere is investigated by conducting a three-dimensional multispecies magnetohydrodynamic (MHD) model, in which the Venusian ionosphere is developed self-consistently by considering chemical reactions among four major ion species (H ^+ , O _2 ^+ , O ^+ , and CO _2 ^+ ). Based on this developed MHD model, we mainly study the effects of the impulsive solar wind dynamic pressure on the interaction process. Simulation results reveal that the locations of the bow shock and magnetic pileup boundary show an abrupt compression, then expansion, and finally shrinkage to reach a new steady state with the influence of the impulsive dynamic pressure. The recovery time of the large-scale magnetic field is a few minutes. In addition, the peak escape fluxes are enhanced by about 1 order of magnitude due to the increased solar wind dynamic pressure pulse.https://doi.org/10.3847/1538-4357/acfca7Venus |
spellingShingle | Yun Li Ruijing Xiong Haoyu Lu Jinbin Cao Tianle Zhu Guokan Li Shibang Li Influence of an Upstream Dynamic Pressure Pulse on Venus–Solar Wind Interaction by Multispecies Magnetohydrodynamic Simulation The Astrophysical Journal Venus |
title | Influence of an Upstream Dynamic Pressure Pulse on Venus–Solar Wind Interaction by Multispecies Magnetohydrodynamic Simulation |
title_full | Influence of an Upstream Dynamic Pressure Pulse on Venus–Solar Wind Interaction by Multispecies Magnetohydrodynamic Simulation |
title_fullStr | Influence of an Upstream Dynamic Pressure Pulse on Venus–Solar Wind Interaction by Multispecies Magnetohydrodynamic Simulation |
title_full_unstemmed | Influence of an Upstream Dynamic Pressure Pulse on Venus–Solar Wind Interaction by Multispecies Magnetohydrodynamic Simulation |
title_short | Influence of an Upstream Dynamic Pressure Pulse on Venus–Solar Wind Interaction by Multispecies Magnetohydrodynamic Simulation |
title_sort | influence of an upstream dynamic pressure pulse on venus solar wind interaction by multispecies magnetohydrodynamic simulation |
topic | Venus |
url | https://doi.org/10.3847/1538-4357/acfca7 |
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