Formation of supermassive stars in the first stellar clusters: Dependence on the gas temperature

Abstract

The origin of supermassive black holes is an open question that has been explored considering gas- and collision-based formation channels to explain the high number of quasars observed in the early Universe. According to numerical simulations, supermassive stars can be formed in atomic cooling halos when protostars reach accretion rates greater than $\sim 10^{-2}{\mathrm{M}}_{\odot }\mathrm{y}{\mathrm{r}}^{-1}$ and fragmentation is inhibited on parsec scales. It remains uncertain, however, whether fragmentation on smaller scales leads to the formation of a star cluster instead of a supermassive star in the presence of possible cooling mechanisms. We explored the formation of a central massive object through collisions and the accretion of Population III stars in a primordial gas cloud in a gravitationally unstable system by varying the gas temperature and the degree of gravitational instability. We performed multiphysics simulations in the AMUSE framework with a hydrodynamical gas treatment through Smoothed-particle hydrodynamics and $N$-body dynamics for the protostars represented through sink particles. Our results show that central massive objects with masses $\sim 10^4{\mathrm{M}}_{\odot }$ can be formed by accretion and collisions at different temperatures and that the most massive object can reach efficiencies of $\sim 0.61$ for atomic cooling conditions and $\sim 0.95$ for more unstable conditions. We observe a quasi-disk formation for warmer temperatures and a higher contribution through collisions to the mass of a central massive object. Our results show that the embedded cluster is in a supercompetitive accretion regime in which it obtains mass by accretion that is regulated by self-gravity. Our results suggest that in more unstable conditions with lower gas temperatures, a more massive supermassive black hole seed can form.

arXiv comment17 pages, 18 figures, submitted to A&A

References in corpus (86)

• How Massive Single Stars End their Life
• The Nucleosynthetic Signature of Population III
• A luminous quasar at a redshift of z = 7.085
• The Formation of the First Star in the Universe
• An 800-million-solar-mass black hole in a significantly neutral Universe at redshift 7.5
• Formation of the First Supermassive Black Holes
• Formation of Supermassive Black Holes
• An ultra-luminous quasar with a twelve-billion-solar-mass black hole at redshift 6.30
• Thermal and Fragmentation Properties of Star-forming Clouds in Low-metallicity Environments
• Simulations on a Moving Mesh: The Clustered Formation of Population III Protostars
• A Survey of z>5.7 Quasars in the Sloan Digital Sky Survey IV: Discovery of Seven Additional Quasars
• A Luminous Quasar at Redshift 7.642
• The Formation and Fragmentation of Disks around Primordial Protostars
• The Mass Spectrum of the First Stars
• Formation of the first nuclear clusters and massive black holes at high redshift
• Fragmentation of star-forming clouds enriched with the first dust
• Massive black hole seeds from low angular momentum material
• Formation of Primordial Supermassive Stars by Rapid Mass Accretion
• Primordial Star Formation under Far-ultraviolet radiation
• Building up the Population III initial mass function from cosmological initial conditions
• Can Supermassive Black Holes Form in Metal-Enriched High-Redshift Protogalaxies ?
• Low-Mass Relics of Early Star Formation
• Multi-physics simulations using a hierarchical interchangeable software interface
• Black hole formation in the early universe
• Resolving the Formation of Protogalaxies. II. Central Gravitational Collapse
• The Astrophysical Multipurpose Software Environment
• Formation of Massive Primordial Stars: Intermittent UV Feedback with Episodic Mass Accretion
• A multiphysics and multiscale software environment for modeling astrophysical systems
• Limiting Accretion onto Massive Stars by Fragmentation-Induced Starvation
• Titans of the Early Universe: The Prato Statement on the Origin of the First Supermassive Black Holes
• Rapidly Accreting Supergiant Protostars: Embryos of Supermassive Black Holes?
• The aftermath of the first stars: massive black holes
• The Evolution of Supermassive Population III Stars
• Stellar Collisions and the Interior Structure of Blue Stragglers
• SMBH Formation via Gas Accretion in Nuclear Stellar Clusters
• On the number density of "direct collapse" black hole seeds
• Constraining the high redshift formation of black hole seeds in nuclear star clusters with gas inflows
• Massive black hole factories: Supermassive and quasi-star formation in primordial halos
• BRIDGE: A Direct-tree Hybrid N-body Algorithm for Fully Self-consistent Simulations of Star Clusters and their Parent Galaxies
• Subaru High-z Exploration of Low-Luminosity Quasars (SHELLQs). VI. Black Hole Mass Measurements of Six Quasars at 6.1<z<6.7
• Formation of massive protostars in atomic cooling haloes
• Formation of Intermediate-Mass Black Holes through Runaway Collisions in the First Star Clusters
• The Growth of Black Holes from Population III Remnants in the Renaissance Simulations
• Three new VHS-DES Quasars at 6.7 < z < 6.9 and Emission Line Properties at z > 6.5
• The low-end of the black hole mass function at cosmic dawn
• Angular Momentum Transfer and Lack of Fragmentation in Self-Gravitating Accretion Flows
• Formation of massive seed black holes via collisions and accretion
• Supermassive Star Formation via Super Competitive Accretion in Slightly Metal-enriched Clouds
• Collisions in Primordial Star Clusters: Formation Pathway for intermediate mass black holes
• Black hole formation in primordial galaxies: chemical and radiative conditions
• Importance of the Initial Conditions for Star Formation - II. Fragmentation Induced Starvation and Accretion Shielding
• The discovery of a highly accreting, radio-loud quasar at z=6.82
• The importance of magnetic fields for the initial mass function of the first stars
• Periodic bursts of Star Formation in Irregular Galaxies
• A Keplerian disk around Orion Source I, a ~15 Msun YSO
• Binary--single-star scattering VI. Automatic Determination of Interaction Cross Sections
• Substructures in the Keplerian disc around the O-type (proto)star G17.64+0.16
• Supermassive star formation via episodic accretion: protostellar disc instability and radiative feedback efficiency
• Modeling disk fragmentation and multiplicity in massive star formation
• Light, medium-weight or heavy? The nature of the first supermassive black hole seeds
• Evolution of stellar collision products in open clusters. I. Blue stragglers in N-body models of M67
• Making a supermassive star by stellar bombardment
• An improved sink particle algorithm for SPH simulations
• The Distribution of Collisionally Induced Blue Stragglers in the Colour-Magnitude Diagram
• The Mass Distribution of Population III Stars
• Low-Metallicity Protostars and the Maximum Stellar Mass Resulting from Radiative Feedback
• Formation of supermassive stars in the first star clusters
• Growth of intermediate mass black holes by tidal disruption events in the first star clusters
• Formation of supermassive black hole seeds in nuclear star clusters via gas accretion and runaway collisions
• Low density, radiatively inefficient rotating-accretion flow onto a black hole
• Origin of supermassive black holes in massive metal-poor protoclusters
• Rise of the First Super-Massive Stars
• The Formation Rate of Blue Stragglers in 47 Tucanae
• Formation of the first stars
• Forming Pop III binaries in self-gravitating disks: how to keep the orbital angular momentum
• Maximally accreting supermassive stars: a fundamental limit imposed by hydrostatic equilibrium
• Fragmentation inside atomic cooling haloes exposed to Lyman-Werner radiation
• Stellar collisions in flattened and rotating Pop. III star clusters
• Formation of SMBH seeds in Pop III star clusters through collisions : the importance of mass loss
• Global instability by runaway collisions in nuclear stellar clusters: Numerical tests of a route for massive black hole formation
• The effects of a background potential in star cluster evolution: a delay in the relaxation time-scale and runaway collision processes
• Observational Support for Massive Black Hole Formation Driven by Runaway Stellar Collisions in Galactic Nuclei
• On the maximum accretion rate of supermassive stars
• Small-N collisional dynamics III: The battle for the realm of not-so-small-N
• Intermittent fragmentation and statistical variations during gas collapse in magnetised atomic cooling haloes
• The physical origin of super-competitive accretion during the formation of the first supermassive black holes

Cited by in corpus (3)

• Constraints on dynamically-formed massive black holes in Little Red Dots from X-ray non-detections
• Massive star clusters detected by JWST as natural birth places to form intermediate-mass black holes
• Identification of Candidate Halos Hosting Massive Black Hole Seeds in the $\text{Renaissance}$ Simulations with Support Vector Machines