When clusters collide - A numerical Hydro/N-body simulation of merging galaxy clusters

Details When clusters collide - A numerical Hydro/N-body simulation of merging galaxy clusters When clusters collide - A numerical Hydro/N-body simulation of merging galaxy clusters

Apr 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...407l..53r&link_type=abstract

Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 407, no. 2, p. L53-L56.

Statistics

Computation

121

Computational Astrophysics, Digital Simulation, Galactic Clusters, Hydrodynamic Equations, Interacting Galaxies, Intergalactic Media, Gas Density, Gas Temperature, Many Body Problem, X Rays

Scientific paper

A 3D numerical simulation of two merging clusters of galaxies, using a hybrid Hydro/N-body code, is presented. The hydrodynamics of the code is solved by an Eulerian finite difference method. Initial results disclose that the X-ray emission of the dominant cluster becomes elongated and broadened; heating occurs at the core of the dominant cluster as a result of multiple shocks, and high velocity gas motions within the intracluster medium. It is predicted that clusters which have undergone recent mergers and do not have cooling flows will have high peculiar gas velocities and that the shocks and turbulence generated during the merger may power cluster-wide radio halos. Prolonged high-velocity gas motions through the dominant cluster core possibly play a major role in the formation and shaping of wide-angle tailed radio sources associated with central dominant galaxies. The N-body component of the simulation reveals the subcluster to be dispersed as it passes through the dominant cluster.

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