Abstract
The gas and dust in the interstellar medium (ISM) form an essential part of the evolution of galaxies, the formation of stars and planetary systems, and the synthesis of organic molecules that may lead to the emergence of life elsewhere in the Universe. Over their lifetimes, stars return much of their mass to the ISM through winds and supernova explosions, leading to a slow enrichment in heavy elements and dust that form the building blocks from which future generations of stars and planets are made. Stars also inject energy into the ISM via ultraviolet photons, shocks, and wind-blown stellar bubbles. Cosmic rays, x-rays, and ionizing photons influence the ionization state of the gas, whereas shielding by gas and dust leads to the cold, neutral phases of the ISM where molecules can flourish. As a result, the composition and structure of the ISM is governed by a complex interplay of microscopic and macroscopic processes. Understanding this life cycle of gas and dust in the ISM is a key problem in astrophysics, for understanding not only our own Galaxy but also the much more rapid cycling between the ISM and stars in the earliest star-forming galaxies in the Universe (Figure 1).
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Van Dishoeck, E.F., Tielens, A.G.G.M. (2001). Space-borne observations of the life cycle of interstellar gas and dust. In: Bleeker, J.A.M., Geiss, J., Huber, M.C.E. (eds) The Century of Space Science. Springer, Dordrecht. https://doi.org/10.1007/978-94-010-0320-9_27
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