Böhringer / Schuecker / Pratt | Heating versus Cooling in Galaxies and Clusters of Galaxies | Buch | 978-3-642-09257-2 | sack.de

Buch, Englisch, 445 Seiten, Previously published in hardcover, Format (B × H): 155 mm x 235 mm, Gewicht: 709 g

Reihe: ESO Astrophysics Symposia

Böhringer / Schuecker / Pratt

Heating versus Cooling in Galaxies and Clusters of Galaxies

Proceedings of the MPA/ESO/MPE/USM Joint Astronomy Conference held in Garching, Germany, 6-11 August 2006
Softcover version of original hardcover Auflage 2007
ISBN: 978-3-642-09257-2
Verlag: Springer

Proceedings of the MPA/ESO/MPE/USM Joint Astronomy Conference held in Garching, Germany, 6-11 August 2006

Buch, Englisch, 445 Seiten, Previously published in hardcover, Format (B × H): 155 mm x 235 mm, Gewicht: 709 g

Reihe: ESO Astrophysics Symposia

ISBN: 978-3-642-09257-2
Verlag: Springer


The Universe would be a dull and dark place if the gaseous baryons did not cool, collapse, and form stars and galaxies. However, if this gas is allowed to cool unimpeded at the rate predicted from known atomic physics, in the context of a well-established cosmological model, the gaseous matter would form stars and galaxies with a high e?ciency, so that far more than the observed fraction of about 10–15% of the baryonic matter would be found in luminous stellar systems. Therefore,cooling must be damped or regulatedby heating processes, and observations show that this ‘feedback’ is a widespread astrophysical phenomenon. The place where this cooling and feedback manifests itself most dram- ically is in the inner regions of the most massive Dark Matter halos found in our Universe, in the cores of galaxy clusters. The e?ect of cosmic co- ing in these objects was recognized in the mid-1970s, and the term ‘cooling ?ow’ was introduced by Andy Fabian and colleagues at Cambridge as a p- sible explanation of the physical processes obtained in the central regions of clusters. The name refers to the fact that gas cooling in the inner regions is associated with a loss of central pressure, causing an in?ow of hot gas from larger radii.

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Research

Weitere Infos & Material


Observations of Cooling Cores.- AGN-ICM Interaction in Cool Cores.- Cooling Cores in Elliptical Galaxies.- Modelling the AGN-ICM Interaction.- Entropy Structures.- Chemical Abundances in Cool Cores.- Optical and Sub-mm Observations of Cool Cores.- Numerical Simulations and Cosmological Applications.- Suzaku Observations.- Heating vs. Cooling in Galaxy Formation.- Conference Summary.



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