Imaging of ionospheric plasma outflow in the magnetosphere: Verification of a new concept |
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| Institution: | 1. Space Sciences Laboratory, University of California, Berkeley, CA 94720, U.S.A.;2. Space Sciences Laboratory, Lockheed Palo Alto Research Laboratories, Palo Alto, CA 94304, U.S.A.;3. Space Environment Laboratory, National Oceanic and Atmospheric Administration, Boulder, CO 80303, U.S.A.;1. Key Laboratory of Electronics and Information Technology for Space System, National Space Science Center, Chinese Academy of Sciences, Beijing 100190, China;2. University of Chinese Academy of Sciences, Beijing 100049, China;3. School of Fundamental Physics and Mathematical Sciences, Hangzhou Institute for Advanced Study, UCAS, Hangzhou 310024, China;4. Taiji Laboratory for Gravitational Wave Universe, Hangzhou 310024, China;5. Key Laboratory of Gravitational Wave Precision Measurement of Zhejiang Province, Hangzhou 310024, China;1. Indian Institute of Geomagnetism, New Panvel, Mumbai, India;2. Department of Physics, University of Bahrain, Bahrain |
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| Abstract: | The distribution of He+, O+, and charge-exchanged auroral protons can be obtained by tomographic deconvolution of resonantly scattered solar 304, 834 and 1216 Å signals, respectively, by these ions in the sunlit magnetosphere. The Doppler shifts of the emission features, if any, can be used to infer the energies of these ions. This concept have been verified for the case of plasmaspheric He+ ions by the Extreme Ultraviolet telescope on board the Apollo-Soyuz mission. Our calculations for the OII834Å line are in agreement with the observations by the STP78-1 satellite experiment. One Spacelab I experiment has observed “hot emissions” near 1216Å which are predicted by the charge exchange of auroral protons with geocoronal neutral hydrogen atoms. We discuss results of a simulation of expected intensities from various observing conditions and describe the design of an instrument capable of verifying the hypothesis. |
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