The Evolution of Internal Shocks in High Velocity Clouds

Details The Evolution of Internal Shocks in High Velocity Clouds The Evolution of Internal Shocks in High Velocity Clouds

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21360902g&link_type=abstract

American Astronomical Society, AAS Meeting #213, #609.02

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Scientific paper

We have calculated the evolution of internal shocks driven into high velocity clouds descending onto the Galactic disk. We include the acceleration of the clouds under gravity, as well as their deceleration by hydrodynamical drag. In our simulations we compute the trajectories of clouds condensing out of the hot ( 100 km/s near the cloud center, while those in clouds located near the solar circle only reach speeds 25 km/s. This results in an observational prediction - infalling clouds at Galactic longitudes 0 < b < 90 and 270 < b < 360 will be more strongly shocked and ionized than clouds at other Galactic longitudes. We find that for a typical cloud condensing out of the halo (n 0.05 per cc) the internal shocks are radiative, and should produce detectable absorption/emission columns of ions. At shock speeds exceeding 180 km/s we find that the ionizing flux from the postshock recombination zone is high enough to fully pre-ionize the gas in the high velocity cloud. This suggests that these clouds are capable of self-regulating their ionization state.

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