Paperback. 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 1015% 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. This volume documents recent developments that have advanced our understanding of the heating and cooling mechanisms in galaxies and galaxy clusters. Chapters detail results from multi-wavelength observations and advances in numerical hydrodynamical simulations. An additional section covers new research findings on feedback and self-regulatory mechanisms during cosmic structure formation in general and in galaxy formation in particular. Shipping may be from our Sydney, NSW warehouse or from our UK or US warehouse, depending on stock availability.

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T�tulo: Heating versus Cooling in Galaxies and Clusters of Galaxies (Paperback)
Editor: Springer-Verlag Berlin and Heidelberg GmbH & Co. KG, Berlin
Fecha de publicaci�n: 2010
Idioma: Ingl�s
ISBN 10: 3642092578
ISBN 13: 9783642092572
Encuadernaci�n: Paperback
Edici�n: 1� Edici�n
Estado: new

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Sinopsis

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.

De la contraportada

The present volume is the record of a recent topical conference on the interplay between heating and cooling processes in galaxies and clusters of galaxies. The volume documents recent progress in our understanding of the dense central regions of these objects. Chapters detail recent results from multiwavelength observations and advances in numerical hydrodynamical simulations. An additional section covers new research on feedback and self-regulatory mechanisms during cosmic structure formation in general, and in galaxy formation in particular.

With reviews and technical papers written by leading scientists, this state-of-the art report will be a valuable and comprehensive source of reference for all astronomers and astrophysicists active in this field.

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