Clumpy and fractal shocks, and the generation of a velocity dispersion in molecular clouds

Details Clumpy and fractal shocks, and the generation of a velocity dispersion in molecular clouds Clumpy and fractal shocks, and the generation of a velocity dispersion in molecular clouds

2006-10-24

arxiv.org/abs/astro-ph/0610720v1

Mon.Not.Roy.Astron.Soc.374:1115-1124,2007

Astronomy and Astrophysics

Astrophysics

11 pages, 17 figures, accepted for publication in MNRAS

Scientific paper

10.1111/j.1365-2966.2006.11227.x

We present an alternative explanation for the nature of turbulence in molecular clouds. Often associated with classical models of turbulence, we instead interpret the observed gas dynamics as random motions, induced when clumpy gas is subject to a shock. From simulations of shocks, we show that a supersonic velocity dispersion occurs in the shocked gas provided the initial distribution of gas is sufficiently non-uniform. We investigate the velocity size-scale relation $\sigma \propto r^{\alpha}$ for simulations of clumpy and fractal gas, and show that clumpy shocks can produce realistic velocity size-scale relations with mean $\alpha \thicksim 0.5$. For a fractal distribution, with a fractal dimension of 2.2 similar to what is observed in the ISM, we find $\sigma \propto r^{0.4}$. The form of the velocity size-scale relation can be understood as due to mass loading, i.e. the post-shock velocity of the gas is determined by the amount of mass encountered as the gas enters the shock. We support this hypothesis with analytical calculations of the velocity dispersion relation for different initial distributions. A prediction of this model is that the line-of sight velocity dispersion should depend on the angle at which the shocked gas is viewed.

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