Formation of supermassive stars in the first star clusters

Abstract

The formation of supermassive stars is believed to be an essential intermediate step for the formation of the massive black hole seeds that become the supermassive black holes powering the quasars observed in the early Universe. Numerical simulations have shown that supermassive stars can form in atomic-cooling halos when protostars reach accretion rates higher than $\sim 10^{-2}$ M${}_{\odot }$ yr${}^{-1}$ and fragmentation is suppressed on pc scales. It is however still uncertain if a supermassive star still emerges when fragmentation occurs at smaller scales and a cluster of stars is formed instead. In this work we explore the problem of massive object formation due to the interplay of collisions and accretion in star clusters at low metallicity. We model a small embedded cluster of accreting protostars following sub-parsec scale fragmentation during the collapse of a primordial gas cloud and follow its evolution by performing $N$-body plus hydrodynamical simulations. Our results show that supermassive stars with 10${}^3$ and 10${}^4$ M${}_{\odot }$ are always formed due to the interplay of collisions and accretion, and in some cases these objects are part of a binary system. The resulting supermassive star is surrounded by tens of smaller stars with typical masses in the range $1$-$100$ M${}_{\odot }$.

arXiv comment16 pages, 20 figures, accepted by MNRAS

References in corpus (85)

• How Massive Single Stars End their Life
• The Nucleosynthetic Signature of Population III
• A luminous quasar at a redshift of z = 7.085
• An 800-million-solar-mass black hole in a significantly neutral Universe at redshift 7.5
• Formation of Supermassive Black Holes
• An ultra-luminous quasar with a twelve-billion-solar-mass black hole at redshift 6.30
• 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
• Formation of Primordial Supermassive Stars by Rapid Mass Accretion
• Primordial Star Formation under Far-ultraviolet radiation
• Fluctuations in the High-Redshift Lyman-Werner Background: Close Halo Pairs as the Origin of Supermassive Black Holes
• Building up the Population III initial mass function from cosmological initial conditions
• Can Supermassive Black Holes Form in Metal-Enriched High-Redshift Protogalaxies ?
• Multi-physics simulations using a hierarchical interchangeable software interface
• Black hole formation in the early universe
• Formation of massive black holes in rapidly growing pre-galactic gas clouds
• The Astrophysical Multipurpose Software Environment
• A multiphysics and multiscale software environment for modeling astrophysical systems
• Titans of the Early Universe: The Prato Statement on the Origin of the First Supermassive Black Holes
• The aftermath of the first stars: massive black holes
• Rapidly Accreting Supergiant Protostars: Embryos of Supermassive Black Holes?
• The Evolution of Supermassive Population III Stars
• Feedback-regulated Super Massive Black Hole Seed Formation
• Stellar Collisions and the Interior Structure of Blue Stragglers
• SMBH Formation via Gas Accretion in Nuclear Stellar Clusters
• 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
• On the Maximum Mass of Accreting Primordial Supermassive Stars
• 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
• Structure and evolution of high-mass stellar mergers
• Formation of Intermediate-Mass Black Holes through Runaway Collisions in the First Star Clusters
• Direct collapse black hole formation from synchronized pairs of atomic cooling halos
• 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
• How realistic UV spectra and X-rays suppress the abundance of direct collapse black holes
• The low-end of the black hole mass function at cosmic dawn
• Cosmological Simulations of Early Blackhole Formation: Halo Mergers, Tidal Disruption, and the Conditions for Direct Collapse
• Formation of massive seed black holes via collisions and accretion
• Supermassive Star Formation via Super Competitive Accretion in Slightly Metal-enriched Clouds
• Formation of primordial supermassive stars by burst accretion
• Collisions in Primordial Star Clusters: Formation Pathway for intermediate mass black holes
• Formation sites of Population III star formation: The effects of different levels of rotation and turbulence on the fragmentation behavior of primordial gas
• The Direct Collapse of a Massive Black Hole Seed Under the Influence of an Anisotropic Lyman-Werner Source
• 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
• Binary--single-star scattering VI. Automatic Determination of Interaction Cross Sections
• Does disk fragmentation prevent the formation of supermassive stars in protogalaxies?
• Radiation hydrodynamics simulations of the formation of direct-collapse supermassive stellar systems
• Supermassive star formation via episodic accretion: protostellar disc instability and radiative feedback efficiency
• 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
• The suppression of direct collapse black hole formation by soft X-ray irradiation
• An improved sink particle algorithm for SPH simulations
• Forming massive seed black holes in high-redshift quasar host progenitors
• Grids of stellar models with rotation: V. Models from 1.7 to 120 Msun at zero metallicity
• The Distribution of Collisionally Induced Blue Stragglers in the Colour-Magnitude Diagram
• Witnessing the birth of a supermassive protostar
• The winds of the hot massive first stars
• Fitting formulae for evolution tracks of massive stars under extreme metal poor environments for population synthesis calculations and star cluster simulations
• Evolution of stellar collision products in open clusters. II. A grid of low-mass collisions
• The Mass Distribution of Population III Stars
• Fragmentation induced starvation in Population III star formation: a resolution study
• Low-Metallicity Protostars and the Maximum Stellar Mass Resulting from Radiative Feedback
• Trapping of HII regions in Population III star formation
• 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
• Origin of supermassive black holes in massive metal-poor protoclusters
• Assembly of supermassive black hole seeds
• The Formation Rate of Blue Stragglers in 47 Tucanae
• Radiation Hydrodynamical Simulations of the Birth of Intermediate-Mass Black Holes in the First Galaxies
• Formation of the first stars
• The formation of protostellar binaries in primordial minihalos
• Formation of SMBH seeds in Pop III star clusters through collisions : the importance of mass loss
• Stellar collisions in flattened and rotating Pop. III star clusters
• Rapidly accreting supermassive stars: reliable determination of the final mass
• Primordial magnetic fields in Population III star formation: a magnetised resolution study
• 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
• Gravitational stability and fragmentation condition for discs around accreting supermassive stars
• Simulating the formation of massive seed black holes in the early Universe. III: The influence of X-rays

Cited by in corpus (23)

• The Science of the Einstein Telescope
• JWST early Universe observations and ΛCDM cosmology
• UNCOVER: 404 Error -- Models Not Found for the Triply Imaged Little Red Dot A2744-QSO1
• Observability of Low-Luminosity AGN in the Early Universe with JWST
• Global instability by runaway collisions in nuclear stellar clusters: Numerical tests of a route for massive black hole formation
• Testing CCC+TL Cosmology with Observed BAO Features
• Rapid formation of a very massive star >50000 $M_{\odot }$ and subsequently an IMBH from runaway collisions. Direct N-body and Monte Carlo simulations of dense star clusters
• Efficiency of black hole formation via collisions in stellar systems: An analysis of data from simulations and observations
• The THESAN-ZOOM project: Population III star formation continues until the end of reionization
• Massive black hole formation in Population III star clusters
• Mergers all the way down: stellar collisions and kinematics of a dense hierarchically forming massive star cluster in a dwarf starburst
• Formation of supermassive stars in the first stellar clusters: Dependence on the gas temperature
• Hungry or Not: How Stellar-Mass Black Holes Grow (or Don't) in Dark Matter Mini-Haloes at High-Resolution
• Halo Mergers Enhance the Growth of Massive Black Hole Seeds
• Evolution of Star Cluster Within Galaxy using Self-consistent Hybrid Hydro/N-body Simulation
• Gravitational collapse at low to moderate Mach numbers: The relationship between star formation efficiency and the fraction of mass in the massive object
• Constraints on dynamically-formed massive black holes in Little Red Dots from X-ray non-detections
• Super-Eddington accretion in high-redshift quasar hosts: Black-hole driven outflows, galaxy quenching, and the nature of little red dots
• Evolution of Size, Mass, and Density of Galaxies Since Cosmic Dawn
• The first stars
• FROST-CLUSTERS -- III. Metallicity-dependent intermediate mass black hole formation by runaway collisions in dense star clusters
• Mass and Spin Growth of Very Massive Stars in Star Clusters Potentially Associated with Little Red Dots
• Massive star clusters detected by JWST as natural birth places to form intermediate-mass black holes