  We present Far Ultraviolet Spectroscopic Explorer (FUSE) observations of a
Balmer filament in the northeast region of the Cygnus Loop supernova remnant.
The data consist of one spectrum obtained through the 30"x30" (LWRS) aperture
and three spectra at adjacent positions obtained through the 4"x20" (MDRS)
aperture. The nonradiative shocks in the region giving rise to these faint
optical filaments produce strong OVI 1032,1038 emission, which is detected in
all the spectra. The OVI emission is resolved by FUSE into a strong component
centered at 0 km/s, and weaker components centered at +/- 140 km/s. The MDRS
spectra allow us to study the variation of OVI emission in the post-shock
structure. We find that the zero velocity emission is associated directly with
the Balmer filament shock, while the high velocity emission comes from a more
uniformly distributed component elsewhere along the line of sight. We also find
that the shocks producing the emission at +/- 140 km/s have velocities between
180 km/s and 220 km/s, if we assume that the ram pressure driving them is the
same as for the zero velocity component shock. In the context of the cavity
model for the Cygnus Loop, the interaction of the blast wave with the spherical
shell that forms most of the cavity wall can naturally give rise to the similar
red and blue-shifted components that are observed.
