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Volume 20, issue 9
Ann. Geophys., 20, 1349–1359, 2002
https://doi.org/10.5194/angeo-20-1349-2002
© Author(s) 2002. This work is distributed under
the Creative Commons Attribution 3.0 License.

Special issue: Xth EISCAT WORKSHOP

Ann. Geophys., 20, 1349–1359, 2002
https://doi.org/10.5194/angeo-20-1349-2002
© Author(s) 2002. This work is distributed under
the Creative Commons Attribution 3.0 License.

  30 Sep 2002

30 Sep 2002

Estimation of the characteristic energy of electron precipitation

C. F. del Pozo, M. J. Kosch, and F. Honary C. F. del Pozo et al.
  • Department Communication Systems, Lancaster University, Lancaster LA1 4YR, UK
  • Correspondence to: C. F. del Pozo
  • (c.del.pozo@lancaster.ac.uk)

Abstract. Data from simultaneous observations (on 13 February 1996, 9 November 1998, and 12 February 1999) with the IRIS, DASI and EISCAT systems are employed in the study of the energy distribution of the electron precipitation during substorm activity. The estimation of the characteristic energy of the electron precipitation over the common field of view of IRIS and DASI is discussed. In particular, we look closely at the physical basis of the correspondence between the characteristic energy, the flux-averaged energy, as defined below, and the logarithm of the ratio of the green-light intensity to the square of absorption. This study expands and corrects results presented in the paper by Kosch et al. (2001). It is noticed, moreover, that acceleration associated with diffusion processes in the magnetosphere long before precipitation may be controlling the shape of the energy spectrum. We propose and test a "mixed" distribution for the energy-flux spectrum, exponential at the lower energies and Maxwellian or modified power-law at the higher energies, with a threshold energy separating these two regimes. The energy-flux spectrum at Tromsø, in the 1–320 keV range, is derived from EISCAT electron density profiles in the 70–140 km altitude range and is applied in the "calibration" of the optical intensity and absorption distributions, in order to extrapolate the flux and characteristic energy maps.

Key words. Ionosphere (auroral ionosphere; particle precipitation; particle acceleration)

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