Low-metallicity star formation and pop III-II transition

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The first stars in the universe were typically very massive, but those near us are not. The metallicity in the star-forming gas is thought to have played a key role in this transition of characteristic stellar mass scale. By studying the evolution of low-metallicity star-forming clouds up to the formation of protostars by way of radiation hydrodynamics with spherical symmetry, we discuss their fragmentation mass scales. The critical metallicity for low-mass fragmentation is in the range of Zcr = 10-6 -10 -5Zȯ. Although the exact value is still unknown due to uncertain dust nature in the early universe, the small value of Z cr means that low-mass star formation begun just after the first episode of metal enrichment. We also evaluate the upper limit on the stellar mass by the stellar feedback. Owing to the higher density in the envelope and thus higher protostellar accretion rate, the upper limit of stellar mass increases toward lower matallicity.

Original languageEnglish
Title of host publicationDeciphering the Ancient Universe with Gamma-Ray Bursts
Number of pages6
Publication statusPublished - 2010
EventInternational Symposium "Deciphering the Ancient Universe with Gamma-Ray Bursts" - Kyoto, Japan
Duration: 2010 Apr 192010 Apr 23

Publication series

NameAIP Conference Proceedings
ISSN (Print)0094-243X
ISSN (Electronic)1551-7616


ConferenceInternational Symposium "Deciphering the Ancient Universe with Gamma-Ray Bursts"


  • Pop II stars
  • Pop III stars
  • Stars formation


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