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Title: FAINT POPULATION III SUPERNOVAE AS THE ORIGIN OF THE MOST IRON-POOR STARS

Abstract

The most iron-poor stars in the Milky Way provide important observational clues to the astrophysical objects that enriched the primordial gas with heavy elements. Among them, the recently discovered iron-deficient star SMSS J031300.36–670839.3 shows a remarkable chemical composition with a non-detection of iron ([Fe/H] <–7.1) and large enhancement of carbon and magnesium relative to calcium. We investigate supernova yields of metal-free (Population III) stars to interpret the abundance pattern observed in this star. We report that the high [C/Ca] and [C/Mg] ratios and upper limits of other elemental abundances are well reproduced with the yields of core-collapse supernovae (which have normal kinetic energies of explosion E of E {sub 51} = E/10{sup 51} erg =1) and hypernovae (E {sub 51} ≥ 10) of Population III 25 M {sub ☉} or 40 M {sub ☉} stars. The best-fit models assume that the explosions undergo extensive matter mixing and fallback, leaving behind a black hole remnant. In these models, Ca is produced by static/explosive O burning and incomplete Si burning in the Population III supernova/hypernova, in contrast to the suggestion that Ca is originated from the hot-CNO cycle during pre-supernova evolution. Chemical abundances of four carbon-rich iron-poor stars with [Fe/H] <–4.5, including SMSS J031300.36–670839.3,more » are consistently explained by faint supernova models with ejected masses of {sup 56}Ni less than 10{sup –3} M {sub ☉}.« less

Authors:
; ; ;  [1]
  1. Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo, Kashiwa, Chiba 277-8583 (Japan)
Publication Date:
OSTI Identifier:
22365083
Resource Type:
Journal Article
Journal Name:
Astrophysical Journal Letters
Additional Journal Information:
Journal Volume: 792; Journal Issue: 2; Other Information: Country of input: International Atomic Energy Agency (IAEA); Journal ID: ISSN 2041-8205
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ASTROPHYSICS; BLACK HOLES; CALCIUM; CARBON; CHEMICAL COMPOSITION; CNO CYCLE; ELEMENT ABUNDANCE; IRON; KINETIC ENERGY; MAGNESIUM; MASS; MILKY WAY; NICKEL 56; STAR EVOLUTION; SUPERNOVAE

Citation Formats

Ishigaki, Miho N., Tominaga, Nozomu, Kobayashi, Chiaki, and Nomoto, Ken'ichi, E-mail: miho.ishigaki@ipmu.jp. FAINT POPULATION III SUPERNOVAE AS THE ORIGIN OF THE MOST IRON-POOR STARS. United States: N. p., 2014. Web. doi:10.1088/2041-8205/792/2/L32.
Ishigaki, Miho N., Tominaga, Nozomu, Kobayashi, Chiaki, & Nomoto, Ken'ichi, E-mail: miho.ishigaki@ipmu.jp. FAINT POPULATION III SUPERNOVAE AS THE ORIGIN OF THE MOST IRON-POOR STARS. United States. doi:10.1088/2041-8205/792/2/L32.
Ishigaki, Miho N., Tominaga, Nozomu, Kobayashi, Chiaki, and Nomoto, Ken'ichi, E-mail: miho.ishigaki@ipmu.jp. Wed . "FAINT POPULATION III SUPERNOVAE AS THE ORIGIN OF THE MOST IRON-POOR STARS". United States. doi:10.1088/2041-8205/792/2/L32.
@article{osti_22365083,
title = {FAINT POPULATION III SUPERNOVAE AS THE ORIGIN OF THE MOST IRON-POOR STARS},
author = {Ishigaki, Miho N. and Tominaga, Nozomu and Kobayashi, Chiaki and Nomoto, Ken'ichi, E-mail: miho.ishigaki@ipmu.jp},
abstractNote = {The most iron-poor stars in the Milky Way provide important observational clues to the astrophysical objects that enriched the primordial gas with heavy elements. Among them, the recently discovered iron-deficient star SMSS J031300.36–670839.3 shows a remarkable chemical composition with a non-detection of iron ([Fe/H] <–7.1) and large enhancement of carbon and magnesium relative to calcium. We investigate supernova yields of metal-free (Population III) stars to interpret the abundance pattern observed in this star. We report that the high [C/Ca] and [C/Mg] ratios and upper limits of other elemental abundances are well reproduced with the yields of core-collapse supernovae (which have normal kinetic energies of explosion E of E {sub 51} = E/10{sup 51} erg =1) and hypernovae (E {sub 51} ≥ 10) of Population III 25 M {sub ☉} or 40 M {sub ☉} stars. The best-fit models assume that the explosions undergo extensive matter mixing and fallback, leaving behind a black hole remnant. In these models, Ca is produced by static/explosive O burning and incomplete Si burning in the Population III supernova/hypernova, in contrast to the suggestion that Ca is originated from the hot-CNO cycle during pre-supernova evolution. Chemical abundances of four carbon-rich iron-poor stars with [Fe/H] <–4.5, including SMSS J031300.36–670839.3, are consistently explained by faint supernova models with ejected masses of {sup 56}Ni less than 10{sup –3} M {sub ☉}.},
doi = {10.1088/2041-8205/792/2/L32},
journal = {Astrophysical Journal Letters},
issn = {2041-8205},
number = 2,
volume = 792,
place = {United States},
year = {2014},
month = {9}
}