Solar cycle variation of “killer” electrons at geosynchronous orbit and electron flux correlation with the solar wind parameters and ULF waves intensity |
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| Institution: | 1. Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia;2. Research Centre for Astrophysics and Geophysics MAS, Ulaanbaatar, Mongolia;3. Irkutsk State Technical University, Irkutsk, Russia;1. Institute of Space and Astronautical Science, Sagamihara, Kanagawa 252 5210, Japan;2. Planetary Exploration Research Center, Chiba Institute of Technology, Chiba, Japan;3. Hokkaido University, Hokkaido, Japan;4. Senshu University, Tokyo, Japan;5. University of Tokyo, Tokyo, Japan;7. Okayama University, Okayama, Japan;1. University of Basilicata, School of Engineering, 10, Ateneo Lucano Street, 85100 Potenza, Italy;2. National Research Council, Institute of Methodologies for Environmental Analysis (IMAA), c/da S.Loja, 85050 Tito Scalo (PZ), Italy;1. Solar System Missions Division, ESA/ESTEC, Noordwijk, Netherlands;2. Office for Support to New Member States, ESA/ESTEC, Netherlands;3. Science Payload Instrument Section, ESA/ESTEC, Netherlands;1. Science and Technology on Aerospace Flight Dynamics Laboratory, Beijing 100094, China;2. Beijing Aerospace Control Center, Beijing 100094, China |
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| Abstract: | To construct models for hazard prediction from radiation belt particles to satellite electronics, one should know temporal behavior of the particle fluxes. We analyzed 11-year variation in relativistic electron flux (E>2 MeV) at geosynchronous orbit using measurements made by GOES satellites during the 23rd sunspot cycle. As it is believed that electron flux enhancements are connected with the high-speed solar wind streams and ULF or/and VLF activity in the magnetosphere, we studied also solar cycle changes in rank order cross-correlation of the outer radiation belt electron flux with the solar wind speed and both interplanetary and on-ground wave intensity. Data from magnetometers and plasma sensors onboard the spacecraft ACE and WIND, as well as magnetic measurements at two mid-latitude diametrically opposite INTERMAGNET observatories were used. Results obtained show that average value of relativistic electron flux at the decay and minimum phases of solar activity is one order higher than the flux during maximum sunspot activity. Of all solar wind parameters, only solar wind speed variation has significant correlation with changes in relativistic electron flux, taking the lead over the latter by 2 days. Variations in ULF amplitude advance changes in electron flux by 3 days. Results of the above study may be of interest for model makers developing forecast algorithms. |
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| Keywords: | ULF oscillations Energetic electrons Solar wind Solar cycle variations Magnetosphere Radiation belts |
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