  The paradigm for Anomalous X-ray Pulsars (AXPs) has evolved recently with the
discovery by INTEGRAL and RXTE of flat, hard X-ray components in three AXPs.
These non-thermal spectral components differ dramatically from the steeper
quasi-power-law tails seen in the classic X-ray band in these sources, and can
naturally be attributed to activity in the magnetosphere. Resonant, magnetic
Compton upscattering is a candidate mechanism for generating this new
component, since it is very efficient in the strong fields present near AXP
surfaces. In this paper, results from an inner magnetospheric model for
upscattering of surface thermal X-rays in AXPs are presented, using a kinetic
equation formalism and employing a QED magnetic scattering cross section.
Characteristically flat and strongly-polarized emission spectra are produced by
non-thermal electrons injected in the emission region. Spectral results depend
strongly on the observer's orientation and the magnetospheric locale of the
scattering, which couple directly to the angular distributions of photons
sampled. Constraints imposed by the Comptel upper bounds for these AXPs are
mentioned.
