Abstract
Interstellar gas is widely detected at intermediate velocities, both in H i emission at 21 cm and in optical and ultraviolet observations of trace elements seen in absorption toward distant stars. In the northern hemisphere, the distribution of intermediate-velocity clouds is dominated by several large complexes, and two weaker complexes have been identified recently in the southern hemisphere. Intermediate-velocity clouds are located in the lower Galactic Halo and most of them appear to be falling toward the galactic plane. They display a variety of physical conditions, but abundances consistently indicate grain disruption and a gas composition that is nearly solar. A range of models has been proposed to explain these basic characteristics but, at this time, no single scenario offers a compelling description of the intermediate-velocity cloud observations. Overall, evidence appears to be mounting in favor of identifying at least some of the intermediate-velocity clouds with the return flow of a Galactic Fountain. However, in individual cases, several different processes could also be at work and the relationship, if any, between high- and intermediate-velocity clouds is unclear. Intermediate-velocity clouds are a widespread phenomenon which may well play an important role in the dynamics and evolution of the gaseous component of our Galaxy.
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Elise Albert, C., Danly, L. (2004). Interemdiate-velocity Clouds. In: van Woerden, H., Wakker, B.P., Schwarz, U.J., de Boer, K.S. (eds) High-Velocity Clouds. Astrophysics and Space Science Library, vol 312. Springer, Dordrecht. https://doi.org/10.1007/1-4020-2579-3_4
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