Resolving the Formation of Protogalaxies. III.Feedback from the First Stars Metadata

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  • Main Title Resolving the Formation of Protogalaxies. III.Feedback from the First Stars


  • Author: Wise, John H.
    Creator Type: Personal
  • Author: Abel, Tom
    Creator Type: Personal
  • Author: /KIPAC, Menlo Park
    Creator Type: Personal


  • Sponsor: United States. Department of Energy.
    Contributor Type: Organization


  • Name: Stanford Linear Accelerator Center
    Place of Publication: [Menlo Park, California]
    Additional Info: SLAC


  • Creation: 2007-10-30


  • English


  • Content Description: The first stars form in dark matter halos of masses {approx}10{sup 6}M{sub {circle_dot}} as suggested by an increasing number of numerical simulations. Radiation feedback from these stars expels most of the gas from their shallow potential well of their surrounding dark matter halos. We use cosmological adaptive mesh refinement simulations that include self-consistent Population III star formation and feedback to examine the properties of assembling early dwarf galaxies. Accurate radiative transport is modeled with adaptive ray tracing. We include supernova explosions and follow the metal enrichment of the intergalactic medium. The calculations focus on the formation of several dwarf galaxies and their progenitors. In these halos, baryon fractions in 10{sup 8} M{sub {circle_dot}} halos decrease by a factor of 2 with stellar feedback and by a factor of 3 with supernova explosions. We find that radiation feedback and supernova explosions increase gaseous spin parameters up to a factor of 4 and vary with time. Stellar feedback, supernova explosions, and H{sub 2} cooling create a complex, multi-phase interstellar medium whose densities and temperatures can span up to 6 orders of magnitude at a given radius. The pair-instability supernovae of Population III stars alone enrich the halos with virial temperatures of 10{sup 4} K to approximately 10{sup -3} of solar metallicity. We find that 40% of the heavy elements resides in the intergalactic medium (IGM) at the end of our calculations. The highest metallicity gas exists in supernova remnants and very dilute regions of the IGM.
  • Physical Description: 12 pages


  • Keyword: Feedback
  • STI Subject Categories: 72 Physics Of Elementary Particles And Fields
  • Keyword: Supernovae
  • Keyword: Nonluminous Matter
  • Keyword: Astrophysics,Astro
  • Keyword: Galaxies
  • STI Subject Categories: 71 Classical And Quantum Mechanics, General Physics
  • Keyword: Stars
  • Keyword: Baryons
  • Keyword: Radiations
  • Keyword: Supernova Remnants
  • Keyword: Transport Astrophysics,Astro
  • Keyword: Spin
  • Keyword: Explosions


  • Journal Name: Astrophysical Journal


  • Name: Office of Scientific & Technical Information Technical Reports
    Code: OSTI


  • Name: UNT Libraries Government Documents Department
    Code: UNTGD

Resource Type

  • Article


  • Text


  • Report No.: SLAC-PUB-12923
  • Grant Number: AC02-76SF00515
  • Office of Scientific & Technical Information Report Number: 918965
  • Archival Resource Key: ark:/67531/metadc886234


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