Nucleosynthesis in Primordial Hypernovae

Grimmett, J J; Heger, Alexander; Karakas, Amanda I.; Müller, Bernhard

doi:10.1093/mnras/sty1417

Cited by 21 publications

(36 citation statements)

References 109 publications

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“…Overall, the explosion of the massive Pop III star progenitor of HE 1327−2326 is thus more energetic than previously thought (i.e., a hypernova), in line with more recent studies, such as Grimmett et al (2018). Interestingly, previous work has suggested that only faint mixing and fallback first SNe would seed carbon-enhanced metal-poor (CEMP) stars such as HE 1327−2326, since their host minihalos would be disrupted by any larger energy input (Cooke & Madau 2014).…”

Section: Comparison To Aspherical Sne Modelssupporting

confidence: 86%

“…Our best fit model has an initial mass cut of M cut =1.64 M , outer boundary mixing region mass of M mix = 5.65 M and an ejection factor of f = 0.0002. To increase specifically the zinc yield of a mixing and fallback SNe model, the explosion mechanism was modified such that the matter density is artificially reduced, to mimic a high entropy explosion environment, which is required for increased explosive nucleosynthesis (Maeda & Nomoto 2003;Tominaga et al 2007a,b;Grimmett et al 2018). In this modified framework, elements formed in the deepest layers during the explosion, such as zinc, are (at least partially) mixed upward and then ejected.…”

Section: Comparison To Aspherical Sne Modelsmentioning

confidence: 99%

“…The [Zn/Fe] = 0.80 ± 0.25 obtained in this work for HE 1327−2326 at [Fe/H] = −5.20 ± 0.20 is shown by the blue star and black error bars. Abundance values are extracted from the JINAbase (Abohalima & Frebel 2018). model, large Zn and other iron-peak elemental abundances cannot be obtained (Tominaga 2009;Nomoto et al 2013;Grimmett et al 2018) because a weak explosion energy is required to achieve the extensive fallback (necessary for producing a low iron abundance). On the other hand, in the aspherical bipolar jet explosion model, the high entropy environment along the jets enables large [Zn/Fe] ratios since more Zn is ejected.…”

Section: Introductionmentioning

confidence: 99%

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Evidence for an Aspherical Population III Supernova Explosion Inferred from the Hyper-metal-poor Star HE 1327–2326^∗

Ezzeddine

Frebel

Roederer

et al. 2019

ApJ

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We present observational evidence that an aspherical supernova explosion could have occurred in the first stars in the early universe. Our results are based on the first determination of a Zn abundance in a Hubble Space Telescope/Cosmic Origins Spectrograph high-resolution UV spectrum of a hyper metalpoor (HMP) star, HE 1327−2326, with [Fe/H](NLTE) = −5.2. We determine [Zn/Fe] = 0.80 ± 0.25 from a UV Zn i line at 2138Å, detected at 3.4 σ. Yields of a 25 M aspherical supernova model with artificially modified densities exploding with E = 5 × 10 51 ergs best match the entire abundance pattern of HE 1327−2326. Such high-entropy hypernova explosions are expected to produce bipolar outflows which could facilitate the external enrichment of small neighboring galaxies. This has already been predicted by theoretical studies of the earliest star forming minihalos. Such a scenario would have significant implications for the chemical enrichment across the early universe as HMP Carbon Enhanced Metal-Poor (CEMP) stars such as HE 1327−2326 might have formed in such externally enriched environments.

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Section: Comparison To Aspherical Sne Modelssupporting

confidence: 86%

Section: Comparison To Aspherical Sne Modelsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Evidence for an Aspherical Population III Supernova Explosion Inferred from the Hyper-metal-poor Star HE 1327–2326^∗

Ezzeddine

Frebel

Roederer

et al. 2019

ApJ

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“…Subsequently, it has become common practice to use SN models to infer the properties of the primordial progenitors of the most metal-poor observed stars, both for individual stars (e.g., Heger & Woosley 2010;Hansen et al 2011;Nomoto et al 2013;Ishigaki et al 2014;Bessell et al 2015;Placco et al 2016) and for large samples (Cayrel et al 2004;Fraser et al 2017;Ishigaki et al 2018). Additionally, constraints on the primordial IMF can be inferred from bulk properties of metal-poor stars with semi-analytical models (de Bennassuti et al 2017;Hartwig et al 2018;Tarumi et al 2020a).…”

Section: Introductionmentioning

confidence: 99%

A Minimum Dilution Scenario for Supernovae and Consequences for Extremely Metal-Poor Stars

Magg,

Nordlander,

Glover

et al. 2020

Preprint

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To date no metal-free stars have been identified by direct observations. The most common method of constraining their properties is searching the spectra of the most metal-poor stars for the chemical elements created in the first stars and their supernova. In this approach, modelled supernova yields are compared to the observed abundance patterns in extremely metal-poor stars. The method typically only uses the abundance ratios, i.e., the yields are diluted to the observed level. Following the usual assumption of spherical symmetry we compute a simple lower limit of the mass a supernova can mix with and find that it is consistent with all published simulations of early chemical enrichment in the interstellar medium. For three different cases, we demonstrate that this dilution limit can change the conclusions from the abundance fitting. There is a large discrepancy between the dilution found in simulations of SN explosions in minihaloes and the dilution assumed in many abundance fits. Limiting the dilution can significantly alter the likelihood of which supernovae are possible progenitors of observed CEMP-no stars. In particular, some of the faint, very low-yield SNe, which have been suggested as models for the abundance pattern of SMSS0313-6708, cannot explain the measured metal abundances, as their predicted metal yields are too small by two orders of magnitude. Altogether, the new dilution model presented here emphasizes the need to better understand the mixing and dilution behaviour of aspherical SNe.

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“…VMP DLAs have allowed for an empirically driven approach to quantify the abundances of metals ejected from the first stars. They are complementary to using VMP stars for the same purpose (e.g., Grimmett et al 2018;Ishigaki et al 2018;Griffith et al 2021a, K19). Improvements that would benefit future work us-ing VMP DLAs include increasing the number of elemental abundances measured from VMP DLA spectra so that more abundance ratios can be constrained, and increasing the sample size of VMP DLAs to improve the statistics of the empirical constraints.…”

Section: Discussionmentioning

confidence: 99%

Empirical Constraints on Core Collapse Supernova Yields using Very Metal Poor Damped Lyman Alpha Absorbers

Nuñez,

Kirby,

Steidel

2021

Preprint

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We place empirical constraints on the yields from zero-and low-metallicity core collapse supernovae (CCSNe) using abundances measured in very metal-poor (VMP; [Fe/H] ≤ −2) Damped Lyman Alpha Absorbers (DLAs). For some abundance ratios, VMP DLAs constrain the metal yields of the first SNe more reliably than VMP stars. We compile a large sample of high-S/N VMP DLAs from over 30 years of literature, most with high resolution spectral measurements. We infer the median IMFaveraged CCSNe yield from the median values from the DLA abundance ratios of C, N, O, Al, Si, S, and Fe (with respect to Fe and O). Critically, we assume that the DLAs are metal-poor enough that they represent galaxies in their earliest stages of evolution, when CCSNe are the only nucleosynthetic sources of the metals that we analyze. We compare five sets of widely adopted zero-and low-metallicity theoretical yields to the empirical yields derived in this work. We find that the five theoretical yield sets agree with the DLA yields for [Si/O], [Si/Fe], [S/O], and [S/Fe]. The theoretical models predict a very large range of N yields, and only one of the models, Heger & Woosley (2010, hereafter HW10), reproduced the DLA value of [N/Fe] and [N/O], and only one other model, Limongi & Chieffi (2018, hereafter LC18), reproduced [N/O].We briefly investigate the adoption of a SN explosion landscape (where certain initial stellar masses collapse into black holes without contributing to nucleosynthesis) onto HW10 and find the predictions are comparable to when there is no landscape. On the other hand, fixing explosion energy to progenitor mass results in wide disagreements between the predictions and DLA abundances. We also investigate the adoption of a simple, observationally motivated Initial Distribution of Rotational Velocities (IDROV) for LC18, which has rotation velocity is a free parameter, and find a slight improvement in agreement with the observations.

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Nucleosynthesis in Primordial Hypernovae

Cited by 21 publications

References 109 publications

Evidence for an Aspherical Population III Supernova Explosion Inferred from the Hyper-metal-poor Star HE 1327–2326^∗

Evidence for an Aspherical Population III Supernova Explosion Inferred from the Hyper-metal-poor Star HE 1327–2326^∗

A Minimum Dilution Scenario for Supernovae and Consequences for Extremely Metal-Poor Stars

Empirical Constraints on Core Collapse Supernova Yields using Very Metal Poor Damped Lyman Alpha Absorbers

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Nucleosynthesis in Primordial Hypernovae

Cited by 21 publications

References 109 publications

Evidence for an Aspherical Population III Supernova Explosion Inferred from the Hyper-metal-poor Star HE 1327–2326∗

Evidence for an Aspherical Population III Supernova Explosion Inferred from the Hyper-metal-poor Star HE 1327–2326∗

A Minimum Dilution Scenario for Supernovae and Consequences for Extremely Metal-Poor Stars

Empirical Constraints on Core Collapse Supernova Yields using Very Metal Poor Damped Lyman Alpha Absorbers

Contact Info

Product

Resources

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Evidence for an Aspherical Population III Supernova Explosion Inferred from the Hyper-metal-poor Star HE 1327–2326^∗

Evidence for an Aspherical Population III Supernova Explosion Inferred from the Hyper-metal-poor Star HE 1327–2326^∗