Articles | Volume 16, issue 10
Ann. Geophys., 16, 1308–1321, 1998

Special issue: VIIIe EISCAT

Ann. Geophys., 16, 1308–1321, 1998

  31 Oct 1998

31 Oct 1998

Proton transport model in the ionosphere. 2. Influence of magnetic mirroring and collisions on the angular redistribution in a proton beam

M. Galand1, J. Lilensten2, W. Kofman2, and D. Lummerzheim3 M. Galand et al.
  • 1High Altitude Observatory, National Center for Atmospheric Research, Boulder, Colorado, USA
    Fax: +1 303 497 1589; e-mail:
  • 2Centre d'Etudes des Phénomènes Aléatoires et Géophysiques, St Martin d'Hères, France
  • 3Geophysical Institute, University of Alaska, Fairbanks, Alaska, USA

Abstract. We investigate the influence of magnetic mirroring and elastic and inelastic scattering on the angular redistribution in a proton/hydrogen beam by using a transport code in comparison with observations. H-emission Doppler profiles viewed in the magnetic zenith exhibit a red-shifted component which is indicative of upward fluxes. In order to determine the origin of this red shift, we evaluate the influence of two angular redistribution sources which are included in our proton/hydrogen transport model. Even though it generates an upward flux, the redistribution due to magnetic mirroring effect is not sufficient to explain the red shift. On the other hand, the collisional angular scattering induces a much more significant red shift in the lower atmosphere. The red shift due to collisions is produced 
by <1 -keV protons and is so small as to require an instrumental bandwidth <0.2 nm. This explains the absence of measured upward proton/hydrogen fluxes in the Proton I rocket data because no useable data concerning protons <1 keV are available. At the same time, our model agrees with measured ground-based H-emission Doppler profiles and suggests that previously reported red shift observations were due mostly to instrumental bandwidth broadening of the profile. Our results suggest that Doppler profile measurements with higher spectral resolution may enable us to quantify better the angular scattering in proton aurora.

Key words. Auroral ionosphere · Particle precipitation

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