  We present an observational study about the impacts of the interactions in
the kinematics, stellar populations, and oxygen abundances of the components of
the galaxy pair AM\,2322-821. A fairly symmetric rotation curve for the
companion (AM\,2322B) galaxy with a deprojected velocity amplitude of 110 km
s$^{-1}$ was obtained, and a dynamical mass of $ 1.1 - 1.3 \times 10^{10}
M_{\sun}$ within a radius of 4 kpc was estimated using this deprojected
velocity. Asymmetries in the radial velocity field were detected for the
companion, very likely due the interaction between the galaxies. The
interaction between the main and companion galaxies was modelled using
numerical N-body/hydrodynamical simulations, with the result indicating that
the current stage of the system would be about 90 Myr after perigalacticum. The
spatial variation in the distribution of the stellar-population components in
both galaxies was analysed using the stellar population synthesis code {\sc
STARLIGHT}. The companion galaxy is dominated by a very young (t $ \leq
1\times10^{8}$ yr) population, with the fraction of this population to the
total flux at $\lambda\, 5\,870\, \AA$, increasing outwards in the galaxy disc.
On the other hand, the stellar population of AM\,2322A is heterogeneous along
the slit positions observed. Spatial profiles of oxygen abundance in the
gaseous phase were obtained using the diagnostic diagram R23 vs. [OIII]/[OII],
where we compared the observed values with the ones obtained from
photoionization models.
  Such gradients of oxygen abundance are significantly flatter for this pair of
galaxies than in typical isolated spiral galaxies. This metallicity
distribution is interpreted as the gradients having been destroyed by
interaction-induced gas flows from the outer parts to the centre of the galaxy
