Effectivity of the modified two stream instability operating in the vicinity of Venus |
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| Institution: | 1. Space Research Institute, Austrian Academy of Sciences, Schmiedlstr. 6, A-8042 Graz, Austria;2. Institute for Computational Modelling, Russian Academy of Sciences, 660036 Krasnoyarsk-36, Russia;3. Institute for Theoretical Physics, University of Graz, Universitätsplatz 5, A-8010 Graz, Austria;4. Institute for Geophysics, Astrophysics, and Meteorology, University of Graz, Universitätsplatz 5, A-8010 Graz, Austria;1. Department of Physics and Astronomy, University of California, Los Angeles, CA 90095, USA;2. Mani L. Bhaumik Institute for Theoretical Physics, University of California, Los Angeles, CA 90095, USA;3. Theoretical Division, Los Alamos National Laboratory, Los Alamos, NM 87545, USA;1. Corporate Research & Development Center, Toshiba Corporation, 1 Komukai-Toshiba-cho, Saiwai-ku, Kawasaki 212-8582, Japan;2. RIKEN Advanced Institute for Computational Science, 7-1-26, Minatojima-minami-machi, Chuo-ku, Kobe, Hyogo 650-0047, Japan;1. Department of Crystallography and Crystal Chemistry, Moscow State University, 119992 GSP-2 Moscow, Russia;2. Center for Optical Materials and Technologies, Belarusian National Technical University, 65 Nezavisimosti Avenue, Building 17, Minsk, Belarus;1. Department of Physics, Faculty of Science, King Khalid University, P.O. Box 9004, Abha 61413, Saudi Arabia;2. Faculty of Science-AL Faisaliah, Campus, King Abdulaziz University, P.O. Box 80200, Jeddah 21589, Saudi Arabia;3. Nano-Science & Semiconductor Labs., Thin Film Lab., Department of Physics, Faculty of Education, Ain Shams University, Roxy, Cairo, Egypt;1. Materials Processing Division, Bhabha Atomic Research Centre, Trombay, Mumbai 400 085, India;2. Superconductivity & Cryogenics Division, National Physical Laboratory, Dr. K. S. Krishnan Marg, New Delhi 110 012, India;3. Surface Engineering Division, National Aerospace Laboratories, Bangalore 560 017, India |
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| Abstract: | This paper is devoted to the application of the modified two stream or cross current instability (MTSI) to the interaction of the solar wind and Venus. Two scenarios are presented providing favorable conditions for the excitation of the instability. For the first scenario, the free energy source of the MTSI is a significant gradient drift of the solar wind protons near the subsolar ionopause. The corresponding growth rates and frequencies of the MTSI are calculated within a full electromagnetic approach for a two-component plasma. The driving source of the second considered scenario consists in the relative drift velocity between solar wind and planetary particles. For modelling this situation, the dispersion equation for a four-component plasma is solved numerically. |
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