2014ApJ...792L..32I -
Astrophys. J., 792, L32 (2014/September-2)
Faint population III supernovae as the origin of the most iron-poor stars.
ISHIGAKI M.N., TOMINAGA N., KOBAYASHI C. and NOMOTO K.
Abstract (from CDS):
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 E51= E/1051 erg =1) and hypernovae (E51 ≥ 10) of Population III 25 M☉ or 40 M☉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 56Ni less than 10–3 M☉.
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Journal keyword(s):
stars: abundances - stars: Population III - supernovae: general
Simbad objects:
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