Abstract
Abstract. The relativistic electron response in the outer radiation belt during magnetic storms has been studied in relation to solar wind and geomagnetic parameters during the first six months of 1995, a period in which there were a number of recurrent fast solar wind streams. The relativistic electron population was measured by instruments on board the two microsatellites, STRV-1a and STRV-1b, which traversed the radiation belt four times per day from L ~ 1 out to L ~ 7 on highly elliptical, near-equatorial orbits. Variations in the E > 750 keV and E > 1 MeV electrons during the main phase and recovery phase of 17 magnetic storms have been compared with the solar wind speed, interplanetary magnetic field z-component, Bz , the solar wind dynamic pressure and Dst *. Three different types of electron responses are identified, with outcomes that strongly depend on the solar wind speed and interplanetary magnetic field orientation during the magnetic storm recovery phase. Observations also confirm that the L-shell, at which the peak enhancement in the electron count rate occurs has a dependence on Dst *.Key words. Magnetospheric physics (energetic particles, trapped; storms and substorms) – Space plasma physics (charged particle motion and accelerations)
Highlights
The dynamics of the relativistic electron population (E > 0.5 MeV) in the Earth’s outer radiation belt (3 < L < 7) during magnetic storms is not well understood (e.g. Li and Temerin, 2001)
Our study shows that the behaviour of the relativistic electron population can take three distinctly different forms, which are strongly correlated with the solar wind conditions during the storm recovery phase
Reeves (1998) examined the relationship between the relativistic electron population and magnetic storms during the interval 1992–5, using a detector on the geosynchronous satellite 1989-046. He found that every relativistic electron flux enhancement coincided with a magnetic storm, not every storm led to an increase in the relativistic electron flux
Summary
The dynamics of the relativistic electron population (E > 0.5 MeV) in the Earth’s outer radiation belt (3 < L < 7) during magnetic storms is not well understood (e.g. Li and Temerin, 2001). The dynamics of the relativistic electron population (E > 0.5 MeV) in the Earth’s outer radiation belt (3 < L < 7) during magnetic storms is not well understood Li and Temerin, 2001). Reeves (1998) examined the relationship between the relativistic electron population and magnetic storms (defined by Dst) during the interval 1992–5, using a detector on the geosynchronous satellite 1989-046. He found that every relativistic electron flux enhancement coincided with a magnetic storm, not every storm led to an increase in the relativistic electron flux. The correlation between the maximum electron flux during a magnetic
Sign-in/Register to view highlights & summary Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
