  When accretion temporarily ceases in the polar AM Her, the emission line
profiles are known to develop several distinct components, whose origin remains
poorly understood. The new low-state spectra reported here have a more
favorable combination of spectral resolution (R~4500), time resolution (~3-min
exposures), and S/N than earlier work, revealing additional details of the
orbital dependence of the line profiles. The central strong feature of H-alpha
is found to be composed of two components of similar strength, one having K~100
km/sec and phased with the motion of the secondary star, the other having
little or no detectable radial velocity variations. We attribute the central
line component to gas near the coupling region, perhaps with a contribution
from irradiation of the secondary star. The two satellite components have RV
offsets of ~+/-250 km/sec on either side of the central strong H-alpha peak.
These satellites most likely arise in large loops of magnetically confined gas
near the secondary star due to magnetic activity on the donor star and/or
interactions of the magnetic fields of the two stars. Doppler maps show that
these two satellite features have concentrations at velocities that match the
velocity locations of L4 and L5 in the system.
