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

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

Feb 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012apj...745..105w&link_type=abstract

The Astrophysical Journal, Volume 745, Issue 2, article id. 105 (2012).

Astronomy and Astrophysics

Astronomy

Galaxies: Formation, Galaxies: Interactions, Galaxies: Kinematics And Dynamics

Scientific paper

Axisymmetric ring systems can be identified from the new catalog of collisional ring galaxies by Madore et al. in 2009. These are O-type-like collisional ring galaxies. Head-on collisions by dwarf galaxies moving along the symmetric axis were performed through N-body simulations to address their origins. It was found that the simulations with smaller initial relative velocities between two galaxies, or in the cases with heavier dwarf galaxies, could produce rings with higher density contrasts. There is more than one generation of rings in one collision and the lifetime of any generation of rings is about one dynamical time. It was concluded that head-on penetrations could explain these O-type-like ring galaxies identified from the new catalog by Madore et al. in 2009, and the simulated rings resembling the observational O-type-like collisional rings are those at the early stage of one of the ring generations.

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