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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Main Authors: Yun Li, Ruijing Xiong, Haoyu Lu, Jinbin Cao, Tianle Zhu, Guokan Li, Shibang Li
Format: Article
Language:English
Published: IOP Publishing 2023-01-01
Series:The Astrophysical Journal
Subjects:
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.
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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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