  A detailed study of the mixed-morphology galaxy pair CPG 29 (Arp 119, VV 347)
shows spectacular spectroscopic peculiarities in the southern (spiral)
component (Mkn 984) including a spatially resolved region, roughly aligned
along the minor axis of the galaxy, with multiple emission-line components
redshifted by as much as 1300 km s$^{-1}$ with respect to the LINER nucleus.
Strong [OI]\l6300 and [SII]\l\l6716,6731 emission suggest shock ionization. The
rest of the galaxy's disk is spectroscopically undistinguished, with emission
lines characteristic of disk H II regions and, in large part, ordered rotation.
We discuss the following four possible explanations for the morphological and
spectroscopic peculiarities in the spiral: (1) a super--wind scenario,
supported by the high FIR luminosity of the spiral, and by emission line
activity similar to that observed in FIR strong galaxies; (2) motion of the
spiral through a hot, relatively dense intergalactic medium, possibly
associated with the elliptical, that could affect the star formation rate and
create a brightened disk rim; (3) a faint companion in direct collision with
the disk, at $\Delta v_r \sim 1000$ \kms, that would straightforwardly explain
the existence of the different redshift systems; (4) a pole on collision by the
elliptical, that could produce the disturbed morphology and other properties of
the spiral. The elliptical/spiral pole--on collision explains the high velocity
line emitting regions as tidally stripped gas, and accounts for the presence of
gas ionized by moterate velocity shocks. The morphology of Mrk 984 is
consistent
