Mass-loading at Venus: Theoretical expectations |
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| Institution: | 1. Biogeochemistry Research Centre, Plymouth University, Drake Circus, Plymouth PL4 8AA, UK;2. Atkins Limited, 500, Park Avenue, Aztec West, Almondsbury, Bristol BS32 4RZ, UK;3. UK Water Industry Research, 8th floor, 50 Broadway, London SW1H 0RG, UK;1. School of Metallurgy and Environment, Central South University, Changsha, 410083, China;2. State Key Laboratory of Environment-friendly Energy Materials, Southwest University of Science and Technology, Mianyang, 621010, China;1. School of Petroleum Engineering, China University of Petroleum, Qingdao, Shandong, 266580, China;2. Key Laboratory of Unconventional Oil & Gas Development (China University of Petroleum (East China)), Ministry of Education, Qingdao, 266580, PR China;1. Department of Applied Chemistry, ZHCET, Faculty of Engineering and Technology, Aligarh Muslim University, Aligarh 202002, India;2. Department of Chemistry, Presidency University, Kolkata 700 073, India;3. Department of Chemistry, College of Science, King Saud University, Riyadh 11451, Saudi Arabia;4. Department of Chemistry, Jadavpur University, Kolkata 700 032, India;5. Functional Inorganic Materials Lab (FIML), Department of Chemistry, Aligarh Muslim University, Aligarh 202002, India;1. School of Materials Science & Engineering and Research Institute for Energy Equipment Materials, Hebei University of Technology, Tianjin 300130, China;2. Tianjin Key Laboratory of Materials Laminating Fabrication and Interface Control Technology, Hebei University of Technology, Tianjin 300130, China |
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| Abstract: | Previous theoretical studies of the solar wind interaction with Venus have generally involved gas dynamic models of flow past the impenetrable ionopause obstacle. However, because these studies neglected the effects of planetary ion production or mass-loading in the magnetosheath, they did not accurately reproduce certain observed features such as the position of the bow shock. Recent numerical calculations include a source term in the gas dynamic equations to represent the photoionization of the hot atomic oxygen corona. These produce results which agree more closely with both the measured flared shape of the bow shock and properties of the magnetosheath plasma and magnetic field. The solar wind interaction with Mars is also expected to be affected by mass-loading. These findings emphasize the similarity between the unmagnetized planets and comets. |
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