  Electrons in the Earth's radiation belts can be categorized into three
populations: precipitating, quasi-trapped and trapped. We use data from the
DEMETER and SAMPEX missions and from ground-based neutron monitors (NM) and
sunspot observations to investigate the long-term variation of quasi-trapped
and trapped sub-MeV electrons on different L shells in the inner belt. DEMETER
and SAMPEX measurements span over 17 years and show that at $L \leq 1.14$ the
electron flux is anti-correlated with sunspot number, but proportional to the
cosmic ray intensity represented by NM count rates, which suggests that
electrons at the inner edge of the inner belt are produced by Cosmic Ray Albedo
Neutron Decay (CRAND). The solar cycle variation of cosmic rays increased the
electron flux at $L \leq 1.14$ by a factor of two from solar maximum at 2001 to
solar minimum at 2009. At $L \ge 1.2$, both quasi-trapped and trapped electrons
are enhanced during geomagnetic storms and decay to a background level during
extended quiet times. At $L>2$, quasi-trapped electrons resemble trapped
electrons, with correlation coefficients as high as 0.97, indicating that pitch
angle scattering is the dominant process in this region.
