  We present an observational study about the effects of the interactions in
the kinematics, stellar population and abundances of the components of the
galaxy pair AM2306-721. Rotation curves for the main and companion galaxies
were obtained, showing a deprojected velocity amplitude of 175 km/s and 185
km/s, respectively. The interaction between the main and companion galaxies was
modeled using numerical N-body/hydrodynamical simulations, with the result
indicating that the current stage of the merger would be about 250 Myr after
perigalacticum. The spatial variation in the distribution of the stellar
population components in both galaxies was analysed by fitting combinations of
stellar population models of different age groups. The central region of main
galaxy is dominated by an old (5-10 Gyr) population, while significant
contributions from a young (200 Myr) and intermediate (1 Gyr) components are
found in the disk, being enhanced in the direction of the tidal features. The
stellar population of the companion galaxy is overall much younger, being
dominated by components with 1 Gyr or less, quite widely spread over the whole
disk. Spatial profiles of the oxygen abundance were obtained from the a grid of
photoionization models using the R23 line ratio. The disk of the main galaxy
shows a clear radial gradient, while the companion galaxy presents an oxygen
abundance relatively homogeneous across the disk. The absence of an abundance
gradient in the secondary galaxy is interpreted in terms of mixing by gas flows
from the outer parts to the center of the galaxy due to the gravitational
interaction with the more massive primary.
