Solar Physics

, Volume 44, Issue 2, pp 485–501

Fast solar electrons, interplanetary plasma and km-wave type-III radio bursts observed from the IMP-6 spacecraft

  • Hector Alvarez
  • Robert P. Lin
  • Samuel J. Bame

DOI: 10.1007/BF00153227

Cite this article as:
Alvarez, H., Lin, R.P. & Bame, S.J. Sol Phys (1975) 44: 485. doi:10.1007/BF00153227


IMP-6 spacecraft observations of low frequency radio emission, fast electrons, and solar wind plasma are used to examine the dynamics of the fast electron streams which generate solar type-III radio bursts. Of twenty solar electron events observed between April, 1971 and August, 1972, four were found to be amenable to detailed analysis. Observations of the direction of arrival of the radio emission at different frequencies were combined with the solar wind density and velocity measurements at 1 AU to define an Archimedean spiral trajectory for the radio burst exciter. The propagation characteristics of the exciter and of the fast electrons observed at 1 AU were then conpared. We find that: (1) the fast electrons excite the radio emission at the second harmonic; (2) the total distance travelled by the electrons was between 30 and 70% longer than the length of the smooth spiral defined by the radio observations; (3) this additional distance travelled is the result of scattering of the electrons in the interplanetary medium; (4) the observations are consistent with negligible true energy loss by the fast electrons.

Copyright information

© D. Reidel Publishing Company 1975

Authors and Affiliations

  • Hector Alvarez
    • 1
  • Robert P. Lin
    • 2
  • Samuel J. Bame
    • 3
  1. 1.Radio Astronomy Observatory, University of MichiganAnn ArborU.S.A.
  2. 2.Space Sciences Laboratory, University of CaliforniaBerkeleyU.S.A.
  3. 3.Los Alamos Scientific LaboratoryLos AlamosU.S.A.

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