This model provides the integral energy and number flux of precipitating auroral electrons for seven levels of magnetic activity (Kp = 0, 1, 2, 3, 4, 5, and 6 and greater). It is based on about 14.1 million spectra (50 eV to 20 keV) from the SSJ/3 detectors on the DMSP F2 and F4 satellites and the CRL-251 detector on the P78-1 satellite. At each level of activity the high-latitude region was separated into 30 zones in corrected geomagnetic latitude (from 50 to 90) and 48 one-half-hour zones in magnetic local time. Epstein transition functions are used to represent the spatial variation, and a Fourier series of order 6 is used to represent the temporal variation resulting in a total of 364 model coefficients. Coefficient sets were determined for the electron energy flux, the number flux, and the Pedersen and Hall conductivities. The latter is found with the help of empirical relationships between the conductivities and the electron energy flux and average energy.
Availability: FORTRAN code may be available from the authors (see Heppner-Maynard-Rich Electric Field Model).
D. A. Hardy, M. S. Gussenhoven, and E. Holeman, A Statistical Model of the Auroral Electron Precipitation, J. Geophys. Res. 90, 4229, 1985.
R. M. Robinson, R. R. Vondrack, K. Miller, T. Dabbs, and D. A. Hardy, On Calculating Ionospheric Conductivities from the Flux and Energy of Precipitating Electrons, J. Geophys. Res. 92, 2565, 1987.
D. A. Hardy, M. S. Gussenhoven, and R. Raistrick, Statistical and Functional Representations of the Pattern of Auroral Energy Flux, Number Flux, and Conductivity, J. Geophys. Res. 92, 12275, 1987.
NASA Official: Dr. Robert McGuire, Head of the Space Physics Data Facility