Chemo-Photometric Models of Ring Galaxies

Abstract

The peculiar ring galaxies are formed as a result of cosmic interaction. An intruder galaxy plunges through the center of a disk galaxy triggering radially expanding density waves on the disk. Here we present results of SPH simulations which focus on the role of different halos (live and analytical) and bulges on the morphology of the target galaxy and on the star formation rate. We find that inside a live triaxial halo arise unfavourable conditions to the development of a ring. Moreover, for same collision, different features appear if the target galaxy is embedded in an analytical halo or endowed with a massive bulge. The presence of a bulge noticeably affects the star formation rate and the dynamical evolution of the interacting system.

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