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Annales Geophysicae An interactive open-access journal of the European Geosciences Union
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Volume 30, issue 1
Ann. Geophys., 30, 163–175, 2012
https://doi.org/10.5194/angeo-30-163-2012
© Author(s) 2012. This work is distributed under
the Creative Commons Attribution 3.0 License.
Ann. Geophys., 30, 163–175, 2012
https://doi.org/10.5194/angeo-30-163-2012
© Author(s) 2012. This work is distributed under
the Creative Commons Attribution 3.0 License.

Regular paper 17 Jan 2012

Regular paper | 17 Jan 2012

Direct observations of the formation of the solar wind halo from the strahl

C. Gurgiolo1, M. L. Goldstein2, A. F. Viñas2, and A. N. Fazakerley3 C. Gurgiolo et al.
  • 1Bitterroot Basic Research, Hamilton, Montana, USA
  • 2Geospace Science Laboratory, Code 673, NASA Goddard Space Flight Center, Greenbelt, MD, USA
  • 3Mullard Space Science Laboratory, University College London, Holmbury St. Mary Dorking, Surrey RH5 6NT, UK

Abstract. Observations of a continual erosion of the strahl and build up of the halo with distance from the sun suggests that, at least in part, the halo may be formed as a result of scattering of the strahl. This hypothesis is supported in this paper by observation of intense scattering of strahl electrons, which gives rise to a proto-halo electron population. This population eventually merges into, or becomes the halo. The fact that observations of intense scattering of the strahl are not common implies that the formation of the halo may not be a continuous process, but one that occurs, in part, in bursts in regions where the conditions responsible for the scattering are optimum.

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