The Formation of Very Massive Stars in Early Galaxies and Implications for Intermediate Mass Black Holes

Regan, John A.; Wise, John H.; Woods, Tyrone E.; Downes, T. P.; O’Shea, Brian W.; Norman, Michael L.

doi:10.21105/astro.2008.08090

Cited by 51 publications

(47 citation statements)

References 94 publications

(136 reference statements)

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“…For our LW-irradiated model (Halo A), Regan et al (2020b) found a 70× relative increase in the total mass of stars by the end of the simulation, with a mass spectrum peaking at ∼ 1000M and reaching ∼ 6000M (as opposed to stellar masses in the range ∼ 10 -200 M for our control case, Halo B). The final total mass (dark matter, gas and stars) of Halo A was M HaloA = 9.3 × 10 7 M (stellar mass: ≈ 90,000M ) and the final total mass of Halo B was M HaloB = 3.7 × 10 6 M (stellar mass: ≈ 1,300M ).…”

Section: Fragmentation Rapid Accretion and Massive Star Formationmentioning

confidence: 70%

“…In order to compare the stellar populations of primordial halos, we draw on 3D hydrodynamic simulations of two primordial halos described in Regan et al (2020b), which themselves were drawn from the original Renaissance simulations of Xu et al (2013aXu et al ( , 2014 and O'Shea et al (2015), to which the interested reader is referred to for further details. Halo A crosses the atomic cooling limit before experiencing central gravitational collapse.…”

Section: Halo Modelsmentioning

confidence: 99%

“…1 (no stars enter such rapid accretion phases in Halo B). As noted in Regan et al (2020b), rapid growth will still greatly inflate the photospheres of those stars which are accreting. This has profound consequences for the anticipated spectra of these primordial stellar populations.…”

Section: Fragmentation Rapid Accretion and Massive Star Formationmentioning

confidence: 99%

“…Recent numerical simulations have shown that a modest LW background, together with dynamical heating from minor and major mergers, can produce a primordial stellar population which is both much more numerous and more massive than that found in Pop III minihalos (Wise et al 2019;Regan et al 2020b). At the same time, the dense gas flows found in such an environment will lead to intermittent episodes of very rapid ( 0.005M /yr) accretion for some stars.…”

mentioning

confidence: 99%

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Some First Stars Were Red: Detecting Signatures of Massive Population III Formation Through Long-Term Stochastic Color Variations

Woods,

Willott,

Regan

et al. 2021

Preprint

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Identifying stars formed in pristine environments (Pop III) within the first billion years is vital to uncovering the earliest growth and chemical evolution of galaxies. Pop III galaxies, however, are typically expected to be too faint and too few in number to be detectable by forthcoming instruments without extremely long integration times and/or extreme lensing. In an environment, however, where star formation is suppressed until a halo crosses the atomic cooling limit (e.g., by a modest Lyman-Werner flux, high baryonic streaming velocities, and/or dynamical heating effects), primordial halos can form substantially more numerous and more massive stars. Some of these stars will in-turn be accreting more rapidly than they can thermally relax at any given time. Using high resolution cosmological zoom-in simulations of massive star formation in high-z halos, we find that such rapidly accreting stars produce prominent spectral features which would be detectable by JWST. The rapid accretion episodes within the halo lead to stochastic reprocessing of 0-20% of the total stellar emission into the rest-frame optical over long timescales, a unique signature which may allow deep observations to identify such objects out to z ∼ 10 − 13 using mid-and wide-band NIRCam colors alone.

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Section: Fragmentation Rapid Accretion and Massive Star Formationmentioning

confidence: 70%

Section: Halo Modelsmentioning

confidence: 99%

Section: Fragmentation Rapid Accretion and Massive Star Formationmentioning

confidence: 99%

mentioning

confidence: 99%

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Some First Stars Were Red: Detecting Signatures of Massive Population III Formation Through Long-Term Stochastic Color Variations

Woods,

Willott,

Regan

et al. 2021

Preprint

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“…A growing number of recent numerical simulations indicate that the formation of multiple very massive stars (e.g., Wise et al 2019;Regan et al 2020) or SMSs (e.g., Latif et al 2020;Patrick et al 2020) was common in primordial, atomic-cooling halos, and that these could be the origin of the first quasars in the Universe. Here, we have shown that secondary disks in these halos form SMSs whose accretion histories can be coupled to those of the stars in the primary disks via tidal interactions.…”

Section: Discussionmentioning

confidence: 99%

On the Formation and Interaction of Multiple Supermassive Stars in Cosmological Flows

Woods¹,

Samuel²,

Whalen³

et al. 2021

Preprint

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Supermassive primordial stars with masses exceeding ∼10 5 M that form in atomically cooled halos are the leading candidates for the origin of high-redshift quasars with z > 6. Recent numerical simulations, however, find that multiple accretion disks can form within a halo, each of which can host a supermassive star. Tidal interactions between the disks can gravitationally torque gas onto their respective stars and alter their evolution. Later, when two satellite disks collide, the two stars can come into close proximity. This may induce additional mass exchange between them. We investigate the co-evolution of supermassive stars in atomically-cooled halos driven by gravitational interactions between their disks. We find a remarkable diversity of evolutionary outcomes. The results depend on these interactions and how the formation and collapse times of the stars in the two disks are correlated. They range from co-evolution as main sequence stars to main sequence -black hole pairs and black hole -black hole mergers. We examine the evolution of these secondary supermassive stars in detail and discuss the prospects for binary interactions on much smaller scales after the disks merge within their host halos.

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Intermediate-mass black holes in star clusters and dwarf galaxies

Askar,

Baldassare,

Mezcua

2024

Black Holes in the Era of Gravitational-Wave Astronomy

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The Formation of Very Massive Stars in Early Galaxies and Implications for Intermediate Mass Black Holes

Cited by 51 publications

References 94 publications

Some First Stars Were Red: Detecting Signatures of Massive Population III Formation Through Long-Term Stochastic Color Variations

Some First Stars Were Red: Detecting Signatures of Massive Population III Formation Through Long-Term Stochastic Color Variations

On the Formation and Interaction of Multiple Supermassive Stars in Cosmological Flows

Intermediate-mass black holes in star clusters and dwarf galaxies

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