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AGN Feedback in Elliptical Galaxies: Numerical Simulations

  • Luca CiottiEmail author
  • Jeremiah P. Ostriker
Chapter
Part of the Astrophysics and Space Science Library book series (ASSL, volume 378)

Abstract

The importance of feedback (radiative and mechanical) from massive black holes at the centers of elliptical galaxies is not in doubt, given the well established relation among black hole mass and galaxy optical luminosity. Here, with the aid of high-resolution hydrodynamical simulations, we discuss how this feedback affects the hot ISM of isolated elliptical galaxies of different mass. The cooling and heating functions include photoionization plus Compton heating, the radiative transport equations are solved, and the mechanical feedback due to the nuclear wind is also described on a physical basis; star formation is considered. In the medium-high mass galaxies the resulting evolution is highly unsteady. At early times major accretion episodes caused by cooling flows in the recycled gas produced by stellar evolution trigger AGN flaring: relaxation instabilities occur so that duty cycles are small enough to account for the very small fraction of massive ellipticals observed to be in the QSO-phase, when the accretion luminosity approaches the Eddington luminosity. At low redshift all models are characterized by smooth, very sub-Eddington mass accretion rates. The mass accumulated by the central black hole is limited to range observed today, even though the mass lost by the evolving stellar population is roughly two order of magnitude larger than the black hole masses observed in elliptical galaxies.

Keywords

Star Formation Stellar Population Elliptical Galaxy Radiative Feedback Galaxy Model 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

Notes

Acknowledgements

We thank Ena Choi, Janfey Jang, Greg Novak, Silvia Pellegrini, Daniel Proga, Sergei Sazonov, Min-Su Shin, Anatoly Spitkovski, Rashid Sunyaev for their precious collaboration in the research effort described in this paper. We also thank Dong-Woo Kim and Silvia Pellegrini for organizing the Joint Discussion at the IAU General Assembly in Rio, and for editing this volume. L.C. is supported by the MIUR Prin2008.

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Copyright information

© Springer New York 2012

Authors and Affiliations

  1. 1.Department of AstronomyUniversity of BolognaBolognaItaly
  2. 2.Princeton University ObservatoryPrincetonUSA
  3. 3.IoAUniversity of CambridgeCambridgeUK

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