Self-similar collapse of collisional gas in an expanding Universe

Details Self-similar collapse of collisional gas in an expanding Universe Self-similar collapse of collisional gas in an expanding Universe

2000-05-16

arxiv.org/abs/astro-ph/0005331v2

Mon.Not.Roy.Astron.Soc.319:797,2000

Astronomy and Astrophysics

Astrophysics

version accepted for publication in the MNRAS

Scientific paper

10.1046/j.1365-8711.2000.03865.x

Similarity solutions are found for the adiabatic collapse of density perturbations $\delta M/M \propto r^{-s}$ $(s>0)$ in a flat universe containing collisional gas only. The solutions are obtained for planar, cylindrical, and spherical perturbations with zero initial pressure. For adiabatic index $\gamma\ge 4/3$, a shock develops at a fixed fraction of the current turnaround distance. Near the center of a spherical perturbations with $\gamma>4/3$ and $s>1/2$, the gas is in quasi-hydrostatic equilibrium (pressure supported) and has an asymptotic power law density profile, $\rho\sim r^{-3s/(s+1)}$, independent of $\gamma$. For $s\le 1/2$, the profile depends on $\gamma$, the pressure is finite, the temperature decreases inward, and gravity dominates pressure causing a continuous inward flow. Although for $1/20$. We also derive the asymptotic behaviour of the gas variables near the center in a universe dominated by collisionless matter. In such a universe, the gas in a spherical perturbation with $s<2$ cannot be pressure supported and the temperature approaches a constant near the center. The solutions and the asymptotic behaviour are relevant for modelling the gas distribution in galaxy clusters and pancake-like superclusters, and determining the structure of haloes of self-interacting dark matter with large interaction cross section.

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