Abstract
AbstractThe past 10 years have seen a resurgence in studies of the Milky Way's interstellar medium (ISM) driven by new surveys of the Galactic plane at wavelengths from 4 microns to 20 cm. These surveys, which include the H I International Galactic Plane Survey, the Spitzer GLIMPSE and MIPSGAL surveys, the recently commenced Herschel HI‐GAL survey, and several surveys of CO J = 1–0, are allowing us to trace the evolution of the ISM on scales of parsecs and sub‐parsecs from warm and diffuse through to cold, dusty molecular gas. Together with hydrodynamical simulations of ever‐increasing sophistication our understanding of the ISM in the disk of the Milky Way has evolved from the 1970's simplistic models of cold clouds surrounded by warm gas to a complex mixture of phases intertwined and interconnected, whose cooling is driven by colliding flows. Here I focus on the “frothy” ISM, where structure and evolution is impacted by bubbles, shells and supershells. I discuss the role of these objects in cooling, the formation of molecules and even the transfer of matter out of the disk of the Galaxy (© 2012 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
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