  We propose that the quiescent emission of AXPs/SGRs is powered by accretion
from a fallback disk, requiring magnetic dipole fields in the range
10^{12}-10^{13} G, and that the luminous hard tails of their X-ray spectra are
produced by bulk-motion Comptonization in the radiative shock near the bottom
of the accretion column. This radiation escapes as a fan beam, which is partly
absorbed by the polar cap photosphere, heating it up to relatively high
temperatures. The scattered component and the thermal emission from the polar
cap form a polar beam. We test our model on the well-studied AXP 4U 0142+61,
whose energy-dependent pulse profiles show double peaks, which we ascribe to
the fan and polar beams. The temperature of the photosphere (kT~0.4 keV) is
explained by the heating effect. The scattered part forms a hard component in
the polar beam. We suggest that the observed high temperatures of the polar
caps of AXPs/SGRs, compared with other young neutron stars, are due to the
heating by the fan beam. Using beaming functions for the fan beam and the polar
beam and taking gravitational bending into account, we fit the energy-dependent
pulse profiles and obtain the inclination angle and the angle between the spin
axis and the magnetic dipole axis, as well as the height of the radiative shock
above the stellar surface. We do not explain the high luminosity bursts, which
may be produced by the classical magnetar mechanism operating in super-strong
multipole fields.
