Astronomy and Astrophysics – Astrophysics
Scientific paper
1997-10-15
Astrophys.J. 496 (1998) 670
Astronomy and Astrophysics
Astrophysics
26 pages, 15 figures included, submitted to ApJ; for color figures and movies see http://www.astro.virginia.edu/~pmr7u/paper_o
Scientific paper
10.1086/305393
We present numerical simulations of off-center collisions between galaxy clusters made using a new hydrodynamical code based on the piecewise-parabolic method (PPM) and an isolated multigrid Poisson solver. We have performed three gas-only high-resolution simulations of collisions between equal-mass clusters with different values of the impact parameter (0, 5, and 10 times the core radius). With these simulations we have studied the observational appearance of the merging clusters and the variation in equilibration time, luminosity enhancement during the collision, and structure of the merger remnant with varying impact parameter. Observational evidence of an ongoing collision is present for 1-2 sound crossing times after the collision, but only for special viewing angles. The remnant actually requires at least five crossing times to reach virial equilibrium. Since the sound crossing time can be as large as 1-2 Gyr, the equilibration time can thus be a large fraction of the age of the universe. The final merger remnant is very similar for impact parameters of zero and five core radii. It possesses a roughly isothermal core, with central density and temperature twice the initial values. Outside the core the temperature drops as r^-1, and the density roughly as r^-3.8. The core radius shows a small increase due to shock heating during the merger. For an impact parameter of ten core radii the core of the remnant possesses a more flattened density profile, with a steeper dropoff outside the core. In both off-center cases the merger remnant rotates, but only for the ten-core-radius case does this appear to have an effect on the structure of the remnant.
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