Decoding the Message From Meteoritic Stardust Silicon Carbide Grains

Lewis, K.; Lugaro, Maria; Gibson, Brad K.; Pilkington, K.

doi:10.1088/2041-8205/768/1/l19

Cited by 32 publications

(40 citation statements)

References 34 publications

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“…This could imply that the AGB stars and SNe that supplied presolar grains had a similar range of initial compositions. This idea is supported by astronomical observations that show that there was essentially no evolution of metallicity in the Milky Way disk during the last 6-7 Gyr (see Lewis et al 2013). Decay of radioactive 32 Si (half-life 153 yr) has been invoked to explain the 32 S excesses observed in SiC SN grains (Pignatari et al 2013).…”

Section: Ab Grains In the Context Of Supernova Modelsmentioning

confidence: 66%

Isotopic Signatures of Supernova Nucleosynthesis in Presolar Silicon Carbide Grains of Type AB with Supersolar ¹⁴N/¹⁵N Ratios

Hoppe

Stancliffe

Pignatari

et al. 2019

ApJ

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We report high-resolution C, N, Al, Si, and S isotope data of 38 presolar SiC grains of type AB. Seventeen of these grains are of subtype AB1 ( 14 N/ 15 N < 440=solar) and 20 of subtype AB2 ( 14 N/ 15 N440), previously proposed to be mainly from supernovae (AB1) and J-type carbon stars (AB2), respectively. Our data are compatible with previously obtained isotope data of AB grains, except that 26 Al/ 27 Al ratios of AB1 grains span a narrower range. The data are compared with predictions from supernova models that consider H ingestion into the He shell during the pre-supernova phase. In these models a mixture of explosive H and He burning occurs at the bottom of the He shell during passage of the supernova shock, forming the so-called O/nova zone. Mixing matter from the O/nova zone with matter from the overlying He/C zone and the stellar envelope shows that the isotopic compositions and trends of both AB1 and AB2 grains can be matched within the model uncertainties. This demonstrates that supernovae should be considered as potential sources of AB2 grains, in addition to J-type carbon stars and born-again asymptotic giant branch stars, as previously proposed.

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Section: Ab Grains In the Context Of Supernova Modelsmentioning

confidence: 66%

Isotopic Signatures of Supernova Nucleosynthesis in Presolar Silicon Carbide Grains of Type AB with Supersolar ¹⁴N/¹⁵N Ratios

Hoppe

Stancliffe

Pignatari

et al. 2019

ApJ

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“…The basis of Galactic chemical evolution is predicated upon theoretical studies of pre-SN stellar evolution, and in particular the predicted yield of a given isotope, much as we have adopted in our earlier work (Gibson 1997;Mishurov et al 2002;Acharova et al 2005aAcharova et al ,b, 2010Acharova et al , 2011Acharova et al , 2012Lewis et al 2013).…”

Section: Methodsmentioning

confidence: 99%

Galactic constraints on supernova progenitor models

Acharova

Gibson

Mishurov

et al. 2013

A&A

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Aims. To estimate the mean masses of oxygen and iron ejected per each type of supernovae (SNe) event from observations of the elemental abundance patterns in the Galactic disk and constrain the relevant SNe progenitor models. Methods. We undertake a statistical analysis of the radial abundance distributions in the Galactic disk within a theoretical framework for Galactic chemical evolution which incorporates the influence of spiral arms. This framework has been shown to recover the non-linear behaviour in radial gradients, the mean masses of oxygen and iron ejected during SNe explosions to be estimated, and constraints to be placed on SNe progenitor models. Results. (i) The mean mass of oxygen ejected per core-collapse SNe (CC SNe) event (which are concentrated within spiral arms) is ∼0.27 M ; (ii) the mean mass of iron ejected by tardy Type Ia SNe (SNeIa, whose progenitors are older/longer-lived stars with ages 100 Myr and up to several Gyr, which do not concentrate within spiral arms) is ∼0.58 M ; (iii) the upper mass of iron ejected by prompt SNeIa (SNe whose progenitors are younger/shorter-lived stars with ages 100 Myr, which are concentrated within spiral arms) is ≤0.23 M per event; (iv) the corresponding mean mass of iron produced by CC SNe is ≤0.04 M per event; (v) short-lived SNe (core-collapse or prompt SNeIa) supply ∼85% of the Galactic disk's iron. Conclusions. The inferred low mean mass of oxygen ejected per CC SNe event implies a low upper mass limit for the corresponding progenitors of ∼23 M , otherwise the Galactic disk would be overabundant in oxygen. This inference is the consequence of the nonlinear dependence between the upper limit of the progenitor initial mass and the mean mass of oxygen ejected per CC SNe explosion. The low mean mass of iron ejected by prompt SNeIa, relative to the mass produced by tardy SNeIa (∼2.5 times lower), prejudices the idea that both sub-populations of SNeIa have the same physical nature. We suggest that, perhaps, prompt SNeIa are more akin to CC SNe, and discuss the implications of such a suggestion.

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“…The predicted isotopic shifts, which include increases in the neutron-rich 29,30 Si, can be compared to measurements of the Si isotopes in pre-solar silicon carbide grains. We refer to Lugaro et al (1999) and references therein for details (see also Zinner et al 2006;Zinner 2008;Lewis et al 2013).…”

Section: From Neon To Ironmentioning

confidence: 99%

The Dawes Review 2: Nucleosynthesis and Stellar Yields of Low- and Intermediate-Mass Single Stars

Karakas

Lattanzio

2014

Publ. Astron. Soc. Aust.

672

675

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The chemical evolution of the Universe is governed by the chemical yields from stars, which in turn are determined primarily by the initial stellar mass. Even stars as low as 0.9 M can, at low metallicity, contribute to the chemical evolution of elements. Stars less massive than about 10 M experience recurrent mixing events that can significantly change the surface composition of the envelope, with observed enrichments in carbon, nitrogen, fluorine, and heavy elements synthesized by the slow neutron capture process (the s-process). Low-and intermediate-mass stars release their nucleosynthesis products through stellar outflows or winds, in contrast to massive stars that explode as core-collapse supernovae. Here we review the stellar evolution and nucleosynthesis for single stars up to ∼10 M from the main sequence through to the tip of the asymptotic giant branch (AGB). We include a discussion of the main uncertainties that affect theoretical calculations and review the latest observational data, which are used to constrain uncertain details of the stellar models. We finish with a review of the stellar yields available for stars less massive than about 10 M and discuss efforts by various groups to address these issues and provide homogeneous yields for low-and intermediate-mass stars covering a broad range of metallicities. Keywords

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Decoding the Message From Meteoritic Stardust Silicon Carbide Grains

Cited by 32 publications

References 34 publications

Isotopic Signatures of Supernova Nucleosynthesis in Presolar Silicon Carbide Grains of Type AB with Supersolar ¹⁴N/¹⁵N Ratios

Isotopic Signatures of Supernova Nucleosynthesis in Presolar Silicon Carbide Grains of Type AB with Supersolar ¹⁴N/¹⁵N Ratios

Galactic constraints on supernova progenitor models

The Dawes Review 2: Nucleosynthesis and Stellar Yields of Low- and Intermediate-Mass Single Stars

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Decoding the Message From Meteoritic Stardust Silicon Carbide Grains

Cited by 32 publications

References 34 publications

Isotopic Signatures of Supernova Nucleosynthesis in Presolar Silicon Carbide Grains of Type AB with Supersolar 14N/15N Ratios

Isotopic Signatures of Supernova Nucleosynthesis in Presolar Silicon Carbide Grains of Type AB with Supersolar 14N/15N Ratios

Galactic constraints on supernova progenitor models

The Dawes Review 2: Nucleosynthesis and Stellar Yields of Low- and Intermediate-Mass Single Stars

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Isotopic Signatures of Supernova Nucleosynthesis in Presolar Silicon Carbide Grains of Type AB with Supersolar ¹⁴N/¹⁵N Ratios

Isotopic Signatures of Supernova Nucleosynthesis in Presolar Silicon Carbide Grains of Type AB with Supersolar ¹⁴N/¹⁵N Ratios