The Formation of the First Massive Black Holes

Chapter
Part of the Astrophysics and Space Science Library book series (ASSL, volume 396)

Abstract

Supermassive black holes (SMBHs) are common in local galactic nuclei, and SMBHs as massive as several billion solar masses already exist at redshift z = 6. These earliest SMBHs may grow by the combination of radiation-pressure-limited accretion and mergers of stellar-mass seed BHs, left behind by the first generation of metal-free stars, or may be formed by more rapid direct collapse of gas in rare special environments where dense gas can accumulate without first fragmenting into stars. This chapter offers a review of these two competing scenarios, as well as some more exotic alternative ideas. It also briefly discusses how the different models may be distinguished in the future by observations with JWST, LISA and other instruments.

Keywords

Black Hole Dark Matter High Redshift Dark Matter Halo Mass Accretion Rate 
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

The author wishes to thank the editors of this volume for their patience during the preparation of this article. I would also like to thank my recent collaborators, especially Taka Tanaka, Cien Shang, Mark Dijkstra and Greg Bryan, whose work was especially emphasized here, and Eliot Quataert for permission to draw on material in our earlier joint review. The work described here was supported in part by the NSF, NASA, and by the Polányi Program of the Hungarian National Office for Research and Technology (NKTH).

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© Springer-Verlag Berlin Heidelberg 2013

Authors and Affiliations

  1. 1.Department of AstronomyColumbia UniversityNew YorkUSA

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