Abstract
Understanding the physical processes that govern the dynamical behavior of the interstellar medium (ISM) is central to much of modern astronomy and astrophysics. The ISM is the primary galactic repository out of which stars are born and into which they deposit energy, momentum and enriched material as they die. It constitutes the anchor point of the galactic matter cycle, and as such is the key to a consistent picture of galaxy formation and evolution. The dynamics of the ISM determines where and when stars form. Similarly, the properties of the planets and planetary systems around these stars are intimately connected to the properties of their host stars and the details of their formation process.
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Notes
- 1.
- 2.
By local, we generally mean within a small volume around the emission site, within which we can assume that physical conditions such as density and temperature do not vary appreciably.
- 3.
Note that this is often referred to in the literature simply as “Lyman-\(\alpha \)” cooling.
- 4.
The chemical energy released when H\(_2\) molecules form on grain surfaces and the direct interaction between dust grains and cosmic rays also affect the grain temperature, but their influence on the mean grain temperature is relatively minor (Leger et al. 1985).
- 5.
This is somewhat smaller than the mean value of \(\sim \) \(20\) K that we quote in Sect. 2.3.2, but this discrepancy is most likely due to our use of the Ossenkopf and Henning (1994) opacities here, as these are intended to represent the behavior of dust in dense molecular clouds and not in the diffuse WNM and CNM.
- 6.
Note that rotational and ro-vibrational emission lines from H\(_2\) have also been detected in the infrared, both in the Milky Way and in other galaxies. However, this emission comes from gas that has been strongly heated by shocks or radiation, and it traces only a small fraction of the total H\(_2\) mass (e.g. van der Werf 2000).
- 7.
The acronym PDR stands for photodissociation region or photon dominated region.
- 8.
- 9.
The latest updates and findings of the research activities on extrasolar planets can be found at the following websites: www.exoplanet.eu and www.exoplanets.org.
- 10.
Information about the Atacama Large Millimeter/Submillimeter Array (ALMA) and about the Gaia satellite can be found at http://www.almaobservatory.org and http://sci.esa.int/gaia/.
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Acknowledgments
Writing these lecture notes would have been impossible without the help and input from many collaborators and colleagues. In particular, we want to thank Christian Baczynski, Javier Ballesteros-Paredes, Robi Banerjee, Erik Bertram, Henrik Beuther, Frank Bigiel, Peter Bodenheimer, Ian A. Bonnell, Andreas Burkert, Paul C. Clark, Cornelis P. Dullemond, Edith Falgarone, Christoph Federrath, Philipp Girichidis, Alyssa Goodman, Dimitrios Gouliermis, Fabian Heitsch, Patrick Hennebelle, Thomas Henning, Mark H. Heyer, Philip F. Hopkins, Juan Ibañez Mejia, Eric R. Keto, Lukas Konstandin, Pavel Kroupa, Mark R. Krumholz, Mordecai-Mark Mac Low, Faviola Molina, Volker Ossenkopf, Thomas Peters, Ralph E. Pudritz, Sarah Ragan, Julia Roman-Duval, Daniel Seifried, Dominik R.G. Schleicher, Wolfram Schmidt, Nicola Schneider, Jennifer Schober, Rahul Shetty, Rowan J. Smith, Jürgen Stutzki, Làszlò Szűcs, Enrique Vazquez-Semadeni, Antony P. Whitworth, and Hans Zinnecker for many stimulating and encouraging discussions.
We acknowledge support from the Deutsche Forschungsgemeinschaft (DFG) via the SFB 881 The Milky Way System (subprojects B1, B2, B5 and B8), and the SPP (priority program) 1573 Physics of the ISM. We also acknowledge substantial support from the European Research Council under the European Community’s Seventh Framework Program (FP7/2007-2013) via the ERC Advanced Grant STARLIGHT: Formation of the First Stars (project number 339177).
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Klessen, R.S., Glover, S.C.O. (2016). Physical Processes in the Interstellar Medium. In: Revaz, Y., Jablonka, P., Teyssier, R., Mayer, L. (eds) Star Formation in Galaxy Evolution: Connecting Numerical Models to Reality. Saas-Fee Advanced Course, vol 43. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-662-47890-5_2
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