Simulation of radiation driven wind from disc galaxies

Abstract

We present 2-D hydrodynamic simulation of rotating galactic winds driven by radiation. We study the structure and dynamics of the cool and/or warm component($T\simeq 10^4$ K) which is mixed with dust. We have taken into account the total gravity of a galactic system that consists of a disc, a bulge and a dark matter halo. We find that the combined effect of gravity and radiation pressure from a realistic disc drives the gas away to a distance of $\sim 5$ kpc in $\sim 37$ Myr for typical galactic parameters. The outflow speed increases rapidly with the disc Eddington parameter ${\Gamma }_0(=\kappa I/(2cG\Sigma )$) for ${\Gamma }_0\ge 1.5$. We find that the rotation speed of the outflowing gas is $\lesssim 100$ km s${}^{-1}$. The wind is confined in a cone which mostly consist of low angular momentum gas lifted from the central region.

10 pages, 11 figures, Accepted for publication in MNRAS

References in corpus (6)

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• On the onset of galactic winds in quiescent star forming galaxies
• Radiation pressure from massive star clusters as a launching mechanism for super-galactic winds
• Warm Molecular Hydrogen in the Galactic Wind of M82
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