Classification of extremely metal-poor stars: Absent region in A(C)-[Fe/H] plane and the role of dust cooling

Gen Chiaki, Nozomu Tominaga, Takaya Nozawa

Research output: Contribution to journalArticlepeer-review

26 Citations (Scopus)

Abstract

Extremely metal-poor (EMP) stars are the living fossils with records of chemical enrichment history at the early epoch of galaxy formation. By the recent large observation campaigns, statistical samples of EMP stars have been obtained. This motivates us to reconsider their classification and formation conditions. From the observed lower limits of carbon and iron abundances of Acr(C) ~6 and [Fe/H]cr ~-5 for C-enhanced EMP (CE-EMP) and C-normal EMP (CN-EMP) stars, we confirm that gas cooling by dust thermal emission is indispensable for the fragmentation of their parent clouds to form such low mass, i.e. long-lived stars, and that the dominant grain species are carbon and silicate, respectively. We constrain the grain radius rcool i of a species i and condensation efficiency fij of a key element j as rcool C /fC,C = 10 μm and rcool Sil /fSil,Mg = 0.1 μm to reproduce Acr(C) and [Fe/H]cr, which give a universal condition 10[C/H]-2.30 + 10[Fe/H] > 10-5.07 for the formation of every EMP star. Instead of the conventional boundary [C/Fe] = 0.7 between CE-EMP and CN-EMP stars, this condition suggests a physically meaningful boundary [C/Fe]b = 2.30 above and below which carbon and silicate grains are dominant coolants, respectively.

Original languageEnglish
Pages (from-to)L115-L119
JournalMonthly Notices of the Royal Astronomical Society: Letters
Volume472
Issue number1
DOIs
Publication statusPublished - 2017 Nov 21
Externally publishedYes

Keywords

  • Dust, extinction
  • Galaxies: Evolution
  • ISM: Abundances
  • Stars: Formation
  • Stars: Low-mass
  • Stars: Population II

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

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