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Mercury Ion Analyzer (MIA) onboard Mercury Magnetospheric Orbiter: MMO
Authors:W Miyake  Y Saito  M Harada  M Saito  H Hasegawa  A Ieda  S Machida  T Nagai  T Nagatsuma  K Seki  I Shinohara  T Terasawa
Institution:1. Department of Aeronautics and Astronautics, Tokai University, 1117 Kitakaname, Hiratsuka, Kanagawa 259-1292, Japan;2. Institute of Space and Astronautical Science, 3-1-1, Yoshinodai, Sagamihara, Kanagawa 229-8510, Japan;3. Solar-Terrestrial Environment Laboratory, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8601, Japan;4. Department of Geophysics, Kyoto University, Oiwake-cho Kitashirakawa Sakyo-Ku Kyoto 606-8502, Japan;5. Department of Earth and Planetary Science, Tokyo Institute of Technology, 12-5 Ookayama 2-12-1 Meguro, Tokyo 152-8551, Japan;6. National Institute of Information and Communications Technology, 4-2-1 Nukui-kita Koganei, Tokyo 184-8795, Japan
Abstract:The Mercury Magnetopsheric Orbiter (MMO) is one of the spacecraft of the BepiColombo mission; the mission is scheduled for launch in 2014 and plans to revisit Mercury with modern instrumentation. MMO is to elucidate the detailed plasma structure and dynamics around Mercury, one of the least-explored planets in our solar system. The Mercury Plasma Particle Experiment (MPPE) on board MMO is a comprehensive instrument package for plasma, high-energy particle, and energetic neutral particle atom measurements. The Mercury Ion Analyzer (MIA) is one of the plasma instruments of MPPE, and measures the three dimensional velocity distribution of low-energy ions (from 5 eV to 30 keV) by using a top-hat electrostatic analyzer for half a spin period (2 s). By combining both the mechanical and electrical sensitivity controls, MIA has a wide dynamic range of count rates for the proton flux expected around Mercury, which ranges from 106 to 1012 cm−2 s−1 str−1 keV−1, in the solar wind between 0.3 and 0.47 AU from the sun, and in both the hot and cold plasma sheet of Mercury’s magnetosphere. The geometrical factor of MIA is variable, ranging from 1.0 × 10−7 cm2 str keV/keV for large fluxes of solar wind ions to 4.7 × 10−4 cm2 str keV/keV for small fluxes of magnetospheric ions. The entrance grid used for the mechanical sensitivity control of incident ions also work to significantly reduce the contamination of solar UV radiation, whose intensity is about 10 times larger than that around Earth’s orbit.
Keywords:BepiColombo  Magnetosphere  Instrumentation
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