A single low-energy, iron-poor supernova as the source of metals in the star SMSS J031300.36−670839.3

Keller, Stefan; Bessell, M. S.; Frebel, Anna; Casey, Andrew R.; Asplund, Martin; Jacobson, Heather R.; Lind, Karin; Norris, John E.; Yong, David; Heger, Alexander; Magic, Zazralt; Costa, G. S. Da; Schmidt, B.; Tisserand, Patrick

doi:10.1038/nature12990

Cited by 359 publications

(422 citation statements)

References 30 publications

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“…These stars are inconsistent with nuclear production of pair-instability supernovae making masses ∼ 140 − 260 M improbable (Keller et al 2014). We have chosen an initial mass of 45M which is expected to collapse into a black hole without SN explosion (Heger et al 2003).…”

Section: D Stellar Evolution Modelmentioning

confidence: 99%

“…SMSS J031300.36-670839.3 (hereafter SMSS J0313-6708, Keller et al 2014), is the most iron-poor star identified at present, with [Fe/H] ≤ −6.53, (Nordlander et al 2017). Li, C, Mg and Ca have been measured and there are upper limits on several other elements.…”

Section: Introductionmentioning

confidence: 99%

“…Li, C, Mg and Ca have been measured and there are upper limits on several other elements. HE 1327-2326 (Frebel et al 2006(Frebel et al , 2008 and HE 1017-5240 (Christlieb E-mail: oclark01@uvic.ca Low-energy or faint supernovae with strong fallback would have either very little or no nucleosynthetic contribution from the supernova explosion (Keller et al 2014;Takahashi et al 2014;Marassi et al 2014). However, many the best fit models proposed for CEMP-no stars are within the mass range where Pop III and the lowest-metallicity stars are expected to collapse directly into black holes with no supernova explosion (Heger et al 2003).…”

Section: Introductionmentioning

confidence: 99%

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Pop III i-process nucleosynthesis and the elemental abundances of SMSS J0313−6708 and the most iron-poor stars

Clarkson

Herwig

Pignatari

2017

Monthly Notices of the Royal Astronomical Society: Letters

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We have investigated a highly energetic H-ingestion event during shell He burning leading to H-burning luminosities of log(L H /L ) ∼ 13 in a 45M Pop III massive stellar model. In order to track the nucleosynthesis which may occur in such an event, we run a series of single-zone nucleosynthesis models for typical conditions found in the stellar evolution model. Such nucleosynthesis conditions may lead to i-process neutron densities of up to ∼ 10 13 cm −3 . The resulting simulation abundance pattern, where Mg comes from He burning and Ca from the i process, agrees with the general observed pattern of the most iron-poor star currently known, SMSS J031300.36-670839.3. However, Na is also efficiently produced in these i process conditions, and the prediction exceeds observations by ∼ 2.5dex. While this probably rules out this model for SMSS J031300.36-670839.3, the typical i-process signature of combined He burning and i process of higher than solar [Na/Mg], [Mg/Al] and low [Ca/Mg] is reproducing abundance features of the two next most iron-poor stars HE 1017-5240 and HE 1327-2326 very well. The i process does not reach Fe which would have to come from a low level of additional enrichment. i process in hyper-metal poor or Pop III massive stars may be able to explain certain abundance patterns observed in some of the most-metal poor CEMP-no stars.

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Section: D Stellar Evolution Modelmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Pop III i-process nucleosynthesis and the elemental abundances of SMSS J0313−6708 and the most iron-poor stars

Clarkson

Herwig

Pignatari

2017

Monthly Notices of the Royal Astronomical Society: Letters

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“…The handful of stars known with [Fe/H] < −5.0 all exhibit large carbonicities (Lee et al 2013;Placco et al 2014b;Frebel & Norris 2015), including the most iron-poor star presently known, SMSS J031300.36-670839.3, with [Fe/H] < −7.5 (Keller et al 2014;Bessell et al 2015). A definitive interpretation of this increasing frequency has not yet been found, but it has been argued (e.g., Carollo et al 2012) that CEMP stars are more frequently associated with the outer-halo population of the Galaxy than with the inner-halo population, suggesting differences in the nucleosynthetic production sites of carbon in these components.…”

Section: Introductionmentioning

confidence: 99%

Abundances of carbon-enhanced metal-poor stars as constraints on their formation

Hansen

Nordström

Hansen

et al. 2016

A&A

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Context. An increasing fraction of carbon-enhanced metal-poor (CEMP) stars is found as their iron abundance, [Fe/H], decreases below [Fe/H] = −2.0. The CEMP-s stars have the highest absolute carbon abundances, [C/H], and are thought to owe their enrichment in carbon and the slow neutron-capture (s-process) elements to mass transfer from a former asymptotic giant branch (AGB) binary companion. The most Fe-poor CEMP stars are normally single, exhibit somewhat lower [C/H] than CEMP-s stars, but show no s-process element enhancement (CEMP-no stars). Abundance determinations of CNO offer clues to their formation sites. Aims. Our aim is to use the medium-resolution spectrograph X-Shooter/VLT to determine stellar parameters and abundances for C, N, Sr, and Ba in several classes of CEMP stars in order to further classify and constrain the astrophysical formation sites of these stars. Methods. Atmospheric parameters for our programme stars were estimated from a combination of V − K photometry, model isochrone fits, and estimates from a modified version of the SDSS/SEGUE spectroscopic pipeline. We then used X-Shooter spectra in conjunction with the 1D local thermodynamic equilibrium spectrum synthesis code MOOG, 1D ATLAS9 atmosphere models to derive stellar abundances, and, where possible, isotopic 12 C/ 13 C ratios. Results. Abundances (or limits) of C, N, Sr, and Ba are derived for a sample of 27 faint metal-poor stars for which the X-Shooter spectra have sufficient signal-to-noise ratios (S/N). These moderate resolution, low S/N (∼10−40) spectra prove sufficient to perform limited chemical tagging and enable assignment of these stars into the CEMP subclasses (CEMP-s and CEMP-no). According to the derived abundances, 17 of our sample stars are CEMP-s and 3 are CEMP-no, while the remaining 7 are carbon-normal. For four CEMP stars, the subclassification remains uncertain, and two of them may be pulsating AGB stars. Conclusions. The derived stellar abundances trace the formation processes and sites of our sample stars. The [C/N] abundance ratio is useful for identifying stars with chemical compositions unaffected by internal mixing, and the [Sr/Ba] abundance ratio allows us to distinguish between CEMP-s stars with AGB progenitors and the CEMP-no stars. Suggested formation sites for the latter include faint supernovae with mixing and fallback and/or primordial, rapidly-rotating, massive stars (spinstars). X-Shooter spectra have thus proved to be valuable tools in the continued search for their origin.

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“…The most iron-poor star found to date, SMSS J031300.36-670839.3 (J031300), by Keller et al (2014); Bessell et al (2015), has an [Fe/H] ratio below 10 −7 . This unusually low iron abundance has been attributed to fallback onto a central black hole (BH) in the weak SN of a 60 M star.…”

Section: Introductionmentioning

confidence: 99%

Low-energy Population III supernovae and the origin of extremely metal-poor stars

Chen

Heger

Whalen

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Some ancient, dim, metal-poor stars may have formed in the ashes of the first supernovae. If their chemical abundances can be reconciled with the elemental yields of specific Pop III explosions, they could reveal the properties of primordial stars. But multidimensional simulations of such explosions are required to predict their yields because dynamical instabilities can dredge material up from deep in the ejecta that would otherwise be predicted to fall back onto the central remnant and be lost in one-dimensional (1D) models. We have performed two-dimensional (2D) numerical simulations of two low-energy Pop III supernovae, a 12.4 M explosion and a 60 M explosion, and find that they produce elemental yields that are a good fit to those measured in the most iron-poor star discovered to date, SMSS J031300.36-670839.3 (J031300). Fallback onto the compact remnant in these weak explosions accounts for the lack of measurable iron in J031300 and its low iron-group abundances in general. Our 2D explosions produce higher abundances of heavy elements (atomic number Z > 20) than their 1D counterparts due to dredge-up by fluid instabilities. Since almost no 56 Ni is ejected by these weak SNe, their low luminosities will prevent their detection in the near infrared with the James Webb Space Telescope and future 30-meter telescopes on the ground. The only evidence that they ever occurred will be in the fossil abundance record.

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A single low-energy, iron-poor supernova as the source of metals in the star SMSS J031300.36−670839.3

Cited by 359 publications

References 30 publications

Pop III i-process nucleosynthesis and the elemental abundances of SMSS J0313−6708 and the most iron-poor stars

Pop III i-process nucleosynthesis and the elemental abundances of SMSS J0313−6708 and the most iron-poor stars

Abundances of carbon-enhanced metal-poor stars as constraints on their formation

Low-energy Population III supernovae and the origin of extremely metal-poor stars

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