Galactic scale gas flows in colliding galaxies: 3-dimensional, N-body/hydrodynamics experiments

Details Galactic scale gas flows in colliding galaxies: 3-dimensional, N-body/hydrodynamics experiments Galactic scale gas flows in colliding galaxies: 3-dimensional, N-body/hydrodynamics experiments

Jun 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994ap%26ss.216..337l&link_type=abstract

Astrophysics and Space Science, vol. 216, no. 1-2, p. 337-346

Statistics

Computation

5

Astronomical Models, Collision Parameters, Computerized Simulation, Disk Galaxies, Elliptical Galaxies, Gas Dynamics, Gas Flow, Interacting Galaxies, Interstellar Gas, Magnetohydrodynamic Flow, Many Body Problem, Star Formation, Computational Fluid Dynamics, Cray Computers, Magnetohydrodynamics, Mathematical Models, Shock Waves, Three Dimensional Models

Scientific paper

We present some results from three dimensional computer simulations of collisions between models of equal mass galaxies, one of which is a rotating, disk galaxy containing both gas and stars and the other is an elliptical containing stars only. We use fully self consistent models in which the halo mass is 2.5 times that of the disk. In the experiments we have varied the impact parameter between zero (head on) and 0.9R (where R is the radius of the disk), for impacts perpendicular to the disk plane. The calculations were performed on a Cray 2 computer using a combined N-body/smooth particle hydrodynamics (SPH) program. The results show the development of complicated flows and shock structures in the direction perpendicular to the plane of the disk and the propagation outwards of a density wave in both the stars and the gas. The collisional nature of the gas results in a sharper ring than obtained for the star particles, and the development of high volume densities and shocks.

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