Journal cover Journal topic
Annales Geophysicae An interactive open-access journal of the European Geosciences Union
Journal topic

Journal metrics

Journal metrics

  • IF value: 1.621 IF 1.621
  • IF 5-year value: 1.614 IF 5-year
    1.614
  • CiteScore value: 1.61 CiteScore
    1.61
  • SNIP value: 0.900 SNIP 0.900
  • SJR value: 0.910 SJR 0.910
  • IPP value: 1.58 IPP 1.58
  • h5-index value: 24 h5-index 24
  • Scimago H <br class='hide-on-tablet hide-on-mobile'>index value: 80 Scimago H
    index 80
Volume 20, issue 7
Ann. Geophys., 20, 957-965, 2002
https://doi.org/10.5194/angeo-20-957-2002
© Author(s) 2002. This work is distributed under
the Creative Commons Attribution 3.0 License.

Special issue: SPACE WEATHER

Ann. Geophys., 20, 957-965, 2002
https://doi.org/10.5194/angeo-20-957-2002
© Author(s) 2002. This work is distributed under
the Creative Commons Attribution 3.0 License.

  31 Jul 2002

31 Jul 2002

The relativistic electron response in the outer radiation belt during magnetic storms

R. H. A. Iles1, A. N. Fazakerley1, A. D. Johnstone1, N. P. Meredith1, and P. Bühler2 R. H. A. Iles et al.
  • 1Mullard Space Science Laboratory, University College London, Holmbury St. Mary, Dorking, Surrey, UK
  • 2Paul Sherrer Institut, Laboratory for Astrophysics, 5232 Villigen PSI, Switzerland
  • Correspondence to: R. H. A. Iles (rhi@mssl.ucl.ac.uk)

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)

Publications Copernicus
Special issue
Download
Citation
Share