Massive black hole factories: Supermassive and quasi-star formation in primordial halos

@article{Schleicher2013MassiveBH,
  title={Massive black hole factories: Supermassive and quasi-star formation in primordial halos},
  author={Dominik R. G. Schleicher and Francesco Palla and Andrea Ferrara and Daniele Galli and Muhammad A. Latif},
  journal={Astronomy and Astrophysics},
  year={2013},
  volume={558}
}
Context. Supermassive stars and quasi-stars (massive stars with a central black hole) are both considered as potential progenitors for the formation of supermassive black holes. They are expected to form from rapidly accreting protostars in massive primordial halos. Aims. We explore how long rapidly accreting protostars remain on the Hayashi track, implying large protostellar radii and weak accretion luminosity feedback. We assess the potential role of energy production in the nuclear core, and… 

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References

SHOWING 1-10 OF 82 REFERENCES
RAPIDLY ACCRETING SUPERGIANT PROTOSTARS: EMBRYOS OF SUPERMASSIVE BLACK HOLES?
Direct collapse of supermassive stars (SMSs) is a possible pathway for generating supermassive black holes in the early universe. It is expected that an SMS could form via very rapid mass accretion
Quasi-stars: accreting black holes inside massive envelopes
We study the structure and evolution of ‘quasi-stars’, accreting black holes embedded within massive hydrostatic gaseous envelopes. These configurations may model the early growth of supermassive
THE GROWTH OF THE STELLAR SEEDS OF SUPERMASSIVE BLACK HOLES
The collapse of baryons into extremely massive stars with masses ≳104 M☉ in a small fraction of protogalaxies at z ≳ 10 is a promising candidate for the origin of supermassive black holes (SMBHs),
Formation of supermassive black holes by direct collapse in pre-galactic haloes
We describe a mechanism by which supermassive black holes (SMBHs) can form directly in the nuclei of protogalaxies, without the need for 'seed' black holes left over from early star formation.
High-redshift formation and evolution of central massive objects - I. Model description
Galactic nuclei host central massive objects either in the form of supermassive black holes or in the form of nuclear stellar clusters. Recent investigations have shown that both components co-exist
The structure and evolution of quasi-stars
The existence of bright quasars at high redshifts implies that supermassive black holes were able to form in the early Universe. Though a number of mechanisms to achieve this have been proposed, none
PROTOSTELLAR FEEDBACK AND FINAL MASS OF THE SECOND-GENERATION PRIMORDIAL STARS
The first stars in the universe ionized the ambient primordial gas through various feedback processes. “Second-generation” primordial stars potentially form from this disturbed gas after its
On the Formation of Massive Primordial Stars
We investigate the formation by accretion of massive primordial protostars in the range of 10-300 M☉. The high accretion rate used in the models ( = 4.4 × 10-3 M☉ yr-1) causes the structure and
Can Supermassive Black Holes Form in Metal-enriched High-Redshift Protogalaxies?
Primordial gas in protogalactic DM halos with virial temperatures Tvir≳ 104 K begins to cool and condense via atomic hydrogen. Provided that this gas is irradiated by a strong UV flux and remains
The First Stellar Cluster
We report results from numerical simulations of star formation in the early universe that focus on gas at very high densities and very low metallicities. We argue that the gas in the central regions
...
...