skip to main content

SciTech ConnectSciTech Connect

Title: THE MASS OF THE FIRST STARS

We perform a three-dimensional radiation hydrodynamics simulation to investigate the formation of the first stars from the initial collapse of a primordial gas cloud to the formation and growth of protostars. The simulation is integrated until {approx}0.1 Myr after the formation of the primary protostar, by which time the protostars have already settled onto the main sequence. This work represents the first attempt at simulating the first episodes of star formation, taking into account the ultraviolet radiative feedback effect from multiple protostars as well as the three-dimensional effects of the fragmentation of the accretion disk. We find that the mass accretion onto Population III protostars is significantly suppressed by their radiative feedback. As a result, we find five stars formed in this particular simulation. The final masses of the stars are {approx}< 60 M{sub Sun }, including a star of 4.4 M{sub Sun }. Formation of such a star hints at the existence of even lower-mass stars that would live today.
Authors:
 [1]
  1. Department of Physics, Konan University, Okamoto, Kobe (Japan)
Publication Date:
OSTI Identifier:
22130955
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astrophysical Journal; Journal Volume: 773; Journal Issue: 2; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ACCRETION DISKS; HYDRODYNAMIC MODEL; MASS; PROTOSTARS; RADIOACTIVE CLOUDS; STARS; THREE-DIMENSIONAL CALCULATIONS; ULTRAVIOLET RADIATION