Summary
We analyse the effects of central AGN heating on the formation of galaxy clusters by means of hydrodynamical simulations. Besides self-gravity of dark matter and baryons, our approach includes radiative cooling and heating processes of the gas component and a multiphase model for a self-consistent treatment of star formation and SNe feedback [1]. Additionally, we incorporate a periodic feedback mechanism in the form of hot buoyant bubbles, injected into the ICM during the active phases of accreting central AGN. We find that AGN heating can substantially affect the properties of the stellar and gaseous components, in particular reducing the mass deposition rate onto the central cD galaxy, thereby offering an energetically plausible solution to the cooling flow problem.
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References
V. Springel, L. Hernquist: MNRAS 339, 289 (2003)
V.Springel: MNRAS 364, 1105 (2005)
D. Sijacki, V. Springel: MNRAS 366, 397-416 (2006)
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© 2007 Springer-Verlag Berlin Heidelberg
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Sijacki, D., Springel, V. (2007). Hydrodynamical Simulations of Cluster Formation withCentral AGN Heating. In: Aschenbach, B., Burwitz, V., Hasinger, G., Leibundgut, B. (eds) Relativistic Astrophysics Legacy and Cosmology – Einstein’s. ESO Astrophysics Symposia. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-540-74713-0_81
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DOI: https://doi.org/10.1007/978-3-540-74713-0_81
Publisher Name: Springer, Berlin, Heidelberg
Print ISBN: 978-3-540-74712-3
Online ISBN: 978-3-540-74713-0
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