Exploratory simulations reveal how gas temperature influences supermassive star formation in primordial clusters, suggesting critical implications for black hole origins.
Key Points
The study examines how gas temperature affects the formation of supermassive stars in primordial stellar clusters.
Performed multiphysics simulations considering a primordial gas cloud with varying gas temperatures.
Evolved a Population III star cluster within a gravitationally unstable system.
Utilized smoothed-particle hydrodynamics and N-body dynamics for protostar representation.
Incorporated physical accretion recipes and realistic mass-radius relations.
Central massive objects reaching ∼10^4 M⊙ formed through collisions and accretion at various temperatures.
The most massive object achieved high formation efficiencies of ∼0.61 under atomic cooling and ∼0.95 in more unstable conditions.
Warmer gas temperatures led to quasi-disk formations and increased contributions from collisions.
Embedded clusters operated in a supercompetitive accretion regime, switching to Bondi-Hoyle accretion at higher temperatures.