Energetic electrons in the magnetotail at 60RE

Energetic electron (Ee>22 kev and Ee>45 kev) observations of the lunar orbiting Explorer 35 satellite from 15 magnetotail crossings at geocentric distances of about 60RE are presented. The longitudinal and latitudinal distributions are shown at two different flux intensities (low fluxes and high fluxes (cutoff J(Ee>22kev) > 345 electrons/cm2 sec ster)). At low fluxes with the counting rate threshold above the cosmic ray background, the occurrence frequency of energetic electrons is almost the same from the dawn side to the dusk side of the tail. The latitudinal distribution shows the occurrence frequency of energetic electrons to be highest near the solar magnetospheric equator and gradual falling off away from the equatorial plane. At high flux levels (J(Ee>22kev) > 345 electrons/cm2 sec ster and J(Ee>45kev) > 278 electrons/cm2 sec ster), the distributions are strongly dependent on longitude and latitude. The occurrence frequency is much higher in the dawn side and near the equator. The region where fluxes were found least frequently is in the northern part of the tail on the dusk side. This dawn to dusk asymmetry appears to increase with increasing flux threshold levels.