  We apply our technique for indirect imaging of the accretion stream to UBVR
eclipse profiles of HU Aqr obtained when the system was in a high state. We
perform model fits to the eclipses using two geometries: one where the stream
accretes onto one footpoint of the field line, and the other where the stream
accretes onto both footpoints. We find that the stream brightness is not
uniform, nor is it a simple function of the radial distance from the white
dwarf. The model provides estimates of the radius where the stream couples to
the magnetic field (1.0-1.3 x10^{10} cm) and of the mass transfer rate (8-76
x10^{16} g/s). We examine the wavelength dependence of the stream brightness,
and find that in the case of the two-footpoint model, the sections of the
magnetically-constrained stream immediately adjacent to the coupling radius
appear to be hotter than the remainder of the stream. This may be due to shock
heating of the plasma as it threads onto the magnetic field.
