Measurements of electron precipitation and ion drift velocities on the spacecraft Atmosphere Explorer C have revealed that electron acceleration regions (or inverted 'V's') in the 1200--1800 MLT quadrant exhibit the following systematic behavior: (1) Electron distribution functions in the acceleration regions are in all cases well described by Maxwellian primary electron beams which have been accelerated through an electrostatic potential V0. (2) The typical inverted V latitudinal structure is always observed in the acceleration regions, with V0 increasing to a maximum and subsequently decreasing to near zero over distances of ~100 to ~ 250 km. (3) In all cases the Maxwellian temperature E0 of the primary electron beam increases systematically with increases in V0. (4) Rather weak acceleration regions, characterized by V0≲1 keV and E0 values of ~100 to ~350 eV, occur in the cusp and in the highest-latitude portion of the dusk side electron precipitation zone, where the ionospheric convection velocity is beginning to rotate from antisunward to sunward. (5) Values of V0 and E0 and the width of the acceleration regions in the cusp and near dusk are similar, this fact together with observation 4 suggesting that both regions are connected to the magnetosheath. (6) Near dusk, regions of much stronger acceleration, characterized by V0 values of ~3 to over 10 keV and E0 values in the ~1-keV range, typically overlap well into the sunward convection region, at times lying completely wihtin it, this behavior suggesting a link with the plasma sheet. (7) The acceleration regions in the sunward convection zone are associated with significant weakening of ionospheric convection velocities relative to the adjacent regions, resulting perhaps from conductivity enhancements produced by the very high electron fluxes that occur within them.