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Axis-symmetric ring systems can be identified from the new catalog ofcollisional ring galaxies in Madore et al. (2009). These are O-type-likecollisional ring galaxies. Head-on collisions by dwarf galaxies moving alongthe symmetric axis were performed through N-body simulations to address theirorigins. It was found that the simulations with smaller initial relativevelocities between two galaxies, or the cases with heavier dwarf galaxies,could produce rings with higher density contrasts. There are more than onegeneration of rings in one collision and the lifetime of any generation ofrings is about one dynamical time. It was concluded that head-on penetrationscould explain these O-type-like ring galaxies identified from the new catalogin Madore et al. (2009), and the simulated rings resembling the observationalO-type-like collisional rings are those at the early stage of one of thering-generations.

The Axis-Symmetric Ring Galaxies: AM 0053-353, AM 0147-350, AM 1133-245, AM 1413-243, AM 2302-322, ARP 318, and Head-On Penetrations