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Formation of the First Stars and Black Holes

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Abstract

We review the current status of knowledge concerning the early phases of star formation during cosmic dawn. This includes the first generations of stars forming in the lowest mass dark matter halos in which cooling and condensation of gas with primordial composition is possible at very high redshift (\(z > 20\)), namely metal-free Population III stars, and the first generation of massive black holes forming at such early epochs, the so-called black hole seeds. The formation of black hole seeds as end states of the collapse of Population III stars, or via direct collapse scenarios, is discussed. In particular, special emphasis is given to the physics of supermassive stars as potential precursors of direct collapse black holes, in light of recent results of stellar evolution models, and of numerical simulations of the early stages of galaxy formation. Furthermore, we discuss the role of the cosmic radiation produced by the early generation of stars and black holes at high redshift in the process of reionization.

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Notes

  1. The accretion efficiency \(\eta \) directly depends on the spin of the black hole, and reaches the maximum value of \(\eta \sim 0.42\) for maximally rotating Kerr black holes. The radiative efficiency \(\epsilon _{r}\) depends both on the type of accretion and on the accretion efficiency: for radiatively efficient accretion events, one can assume \(\epsilon _{r} = \eta \).

  2. Photon losses by LLSs are also due to radiative recombinations. In analytical models it is standard practice, however, to include the effect of LLSs as a reduction in the source term through the finite mean free path of ionizing radiation. Three different quantities – the escape fraction, the gas clumping factor, and the mean free path – are then used to describe what are essentially radiative recombinations in the ISM, the IGM, and the LLSs. Numerical simulations of cosmic reionization show that such a separation into distinct regimes may indeed be reasonable (Kaurov and Gnedin 2015).

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Acknowledgements

The authors thank ISSI for the organisation of the conference at the origin of this review.

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Authors and Affiliations

  1. Département d’Astronomie, Université de Genève, chemin des Maillettes 51, 1290, Geneva, Switzerland

    L. Haemmerlé

  2. Center for Theoretical Astrophysics and Cosmology, Institute for Computational Science, University of Zurich, Winterthurerstrasse 190, 8057, Zurich, Switzerland

    L. Mayer

  3. Zentrum für Astronomie, Institut für Theoretische Astrophysik, Universität Heidelberg, Albert-Ueberle-Str. 2, 69120, Heidelberg, Germany

    R. S. Klessen

  4. Department of Physics, Kyoto University, Kyoto, 606-8502, Japan

    T. Hosokawa

  5. Department of Astronomy and Astrophysics, University of California, 1156 High Street, Santa Cruz, CA, 95064, USA

    P. Madau

  6. Department of Astronomy, The University of Texas at Austin, Austin, TX, 78712, USA

    V. Bromm

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  1. L. Haemmerlé
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  2. L. Mayer
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  3. R. S. Klessen
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  4. T. Hosokawa
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  5. P. Madau
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  6. V. Bromm
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Star Formation

Edited by Andrei Bykov, Corinne Charbonnel, Patrick Hennebelle, Alexandre Marcowith, Georges Meynet, Maurizio Falanga and Rudolf von Steiger

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Haemmerlé, L., Mayer, L., Klessen, R.S. et al. Formation of the First Stars and Black Holes. Space Sci Rev 216, 48 (2020). https://doi.org/10.1007/s11214-020-00673-y

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  • DOI: https://doi.org/10.1007/s11214-020-00673-y

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