Numerical simulations of rotating cooling flows in galaxy cluster environments

Details Numerical simulations of rotating cooling flows in galaxy cluster environments Numerical simulations of rotating cooling flows in galaxy cluster environments

Aug 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998mnras.298..697g&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 298, Issue 3, pp. 697-707.

Astronomy and Astrophysics

Astronomy

2

Hydrodynamics, Instabilities, Galaxies: Clusters: General, Cooling Flows

Scientific paper

We have used 2D numerical simulations to study the evolution of galaxy cluster cooling flows undergoing a rotational perturbation. We show that such rotations in the intracluster medium may arise from cluster/subcluster mergers. Our galaxy cluster initial conditions involve spherically symmetric, steady-state cooling flows with varying mass-dropout strengths. The rotational perturbation serves to break the symmetry for each of the initial cooling flows, resulting in the formation of thin, gaseous disc-like structure extending radially out to ~10 kpc. Disc-like structure formed for low mass-dropout strength simulations appears to contain cooling condensations whereas disc-like structure in higher mass-dropout strength simulations appears smooth. This is due to the influence of mass-dropout on the degree of cooling, which serves to reduce the strength of thermal instabilities by the removal of `cold' gas from the flow. Morphological comparisons of the disc-like structure formed in our simulations are made to structure observed in the X-ray emitting gas of A4059. Comparisons of the gas dynamics within the disc-like structure are also made to the solid-body rotation profile observed from emission-line gas within the central galaxy of Hydra A. The influence of grid effects on the simulations is also discussed.

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