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Where are the high velocity clouds?
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Where are the high velocity clouds?
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Recent observations of high velocity clouds (HVCs) have revealed compression fronts and tail shaped features of HI suggesting that they are interacting with external medium. We perform 3-D hydro-dynamical simulations of HVCs moving through a diffuse hot gaseous component, investigating the behaviour of both extra-galactic dark matter dominated HVCs and nearby pure gas clouds that may be accreting onto the Galactic disk via a Galactic fountain. Both scenarios can give rise to similar features as observed if the external medium has a density $>10^{-4}$ cm$^{-3}$. Observations suggest that this may be too high for a hot ionised halo or intergalactic gas and supports the Galactic fountain origin, a model that can also account for the high fraction of HVCs with tails and asymmetrical morphologies.
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Cited by 1 Pith paper
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Gas accretion onto the Milky Way: high-velocity cloud survival and the revival of the terminal-velocity paradigm
Terminal velocity is a local, conditional equilibrium for Milky Way high-velocity clouds: dense clouds fall quasi-ballistically, adiabatic clouds break up, and radiative cooling can restore terminal-like motion.
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