Speaker
Description
Observational positional and velocity data from two Local Group galaxies, M31 and M33, suggest the possibility of a past interaction between them. This work aims to evaluate the implications of the interaction between the two galaxies in terms of star formation rate of the system, as well of the morphological implications on its stellar disks. Based on recent observational constraints and previous numerical results, the interactive system was modelled and simulated via $N$-body hydrodinamical simulations. Our best simulation suggests the first pericentric passage of the interaction happened $0.96$ Gyr ago, in which the distance between the two galactic centers were of approximately $48.7$ kpc. Preliminary results suggest that the star formation rate does not appear to be significantly affected by the interaction between the two galaxies, even at the moment of closest apporach. The stellar disk morphology, however, suffers relevant warping effects and tidal tail formation.
