Collisions and Mergers of Disk Galaxies: Hydrodynamics of Star Forming Gas

Details Collisions and Mergers of Disk Galaxies: Hydrodynamics of Star Forming Gas Collisions and Mergers of Disk Galaxies: Hydrodynamics of Star Forming Gas

2003-05-23

arxiv.org/abs/astro-ph/0305442v1

Astrophys.Space Sci. 284 (2003) 479-482

Astronomy and Astrophysics

Astrophysics

To be published in Proceedings of 'The Evolution of Galaxies III- From simple approaches to self-consistent models,' held in K

Scientific paper

10.1023/A:1024048009270

We summarize the results of numerical simulations of colliding gas-rich disk galaxies in which the impact velocity is set parallel to the spin axes of the two galaxies. The effects of varying the impact speed are studied with particular attention to the resulting gaseous structures and shockwave patterns, and the time needed to produce these structures. The simulations employ an N-body treatment of the stars and dark matter, together with an SPH treatment of the gas, in which all components of the models are gravitationally active. The results indicate that for such impact geometries, collisions can lead to the very rapid formation of a central, rapidly rotating, dense gas disk, and that in all cases extensive star formation is predicted by the very high gas densities and prevalence of shocks, both in the nucleus and out in the galactic disks. As the dense nucleus is forming, gas and stars are dispersed over very large volumes, and only fall back towards the nucleus over long times. In the case of low impact velocities, this takes an order of magnitude more time than that needed for the formation of a dense nucleus.

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