Beryllium-10 production in gaseous protoplanetary disks and implications for the astrophysical setting of refractory inclusions

Jacquet, Emmanuel

doi:10.1051/0004-6361/201834754

Cited by 22 publications

(10 citation statements)

References 83 publications

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“…Young et al 2008) or nuclear reactions within the Solar System, whether by spallation or radioactive decay (e.g. Lee et al 1998;Gounelle et al 2006;Davis & McKeegan 2014;Sossi et al 2017;Lugaro et al 2018;Jacquet 2019), many bear the stamp of presolar stellar nucleosynthesis. Indeed, deviations from terrestrial standards for elements with numerous isotopes may often be readily interpreted in terms of nucleosynthetic contributions such as the s, r and p processes characteristic of different, if sometimes contentious, types of stars (Dauphas & Schauble 2016;Lugaro et al 2018).…”

Section: Introductionmentioning

confidence: 99%

Fingerprints of the Protosolar Cloud Collapse in the Solar System. II. Nucleosynthetic Anomalies in Meteorites

Jacquet

Pignatale

Chaussidon

et al. 2019

ApJ

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The isotopic heterogeneity of the Solar System shown by meteorite analyses is more pronounced for its earliest objects, the Calcium-Aluminum-rich Inclusions (CAIs). This suggests that it was inherited from spatial variations in different stardust populations in the protosolar cloud. We model the formation of the solar protoplanetary disk following its collapse and find that the solid-weighted standard deviation of different nucleosynthetic contributions in the disk is reduced by one order of magnitude compared to the protosolar cloud, whose successive isotopic signatures are fossilized by CAIs. The enrichment of carbonaceous chondrites in r-process components, whose proportions are inferred to have diminished near the end of infall, is consistent with their formation at large heliocentric distances, where the early signatures would have been preferentially preserved after outward advection. We also argue that thermal processing had little effect on the (mass-independent) isotopic composition of bulk meteorites for refractory elements.

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Section: Introductionmentioning

confidence: 99%

Fingerprints of the Protosolar Cloud Collapse in the Solar System. II. Nucleosynthetic Anomalies in Meteorites

Jacquet

Pignatale

Chaussidon

et al. 2019

ApJ

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“…Beryllium-10, which decays to 10 B with a half-life of 1.4 Ma (Korschinek et al 2010), is produced by spallation reactions induced by galactic and/or stellar cosmic rays (McKeegan et al 2000, Desch et al 2004, Liu et al 2010, Tatischeff et al 2014, Jacquet 2019. The former presence of 10 Be is inferred by anomalous 10 B/ 11 B ratios (relative to the chondritic value of 0.2481, Zhai et al 1996) in phases with high Be/B ratios (such as melilite) in calcium-and aluminiumrich inclusions (CAIs), the first solids formed in the Solar System.…”

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confidence: 99%

“…If 10 Be was homogeneously distributed (i.e., CAIs, which likely formed within a narrow time interval, record a single 10 Be/ 9 Be value), it was likely produced by galactic cosmic rays (GCR) interacting with the molecular cloud core that collapsed to form our Solar System (Desch et al 2004, Tatischeff et al 2014. On the other hand, if 10 Be was distributed heterogeneously (i.e., CAIs display a range of 10 Be/ 9 Be values), 10 Be was likely produced by solar particles interacting with gas and solids in the solar nebula (McKeegan et al 2000, Gounelle et al 2001, MacPherson et al 2003, Jacquet 2019. The origin of 10 Be is currently ambiguous partly because of the difficulty of interpreting the results to date.…”

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confidence: 99%

Best Practices for Determination of Initial ¹⁰Be/⁹Be in Early Solar System Materials by Secondary Ion Mass Spectrometry

Dunham

Desch

Hervig

2020

Geostandard Geoanalytic Res

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Beryllium-10 (t 1/2 = 1.4 Ma) is a short-lived radionuclide present in the early Solar System. It is produced solely by irradiation reactions and can provide constraints on the astrophysical environment of the Sun's formation. Calcium-and aluminium-rich inclusions (CAIs), the first solids formed in the Solar System, show clear evidence for live 10 Be at their time of formation, but it is unclear whether they record the same initial 10 Be/ 9 Be ratio. In this study, we examine the secondary ion mass spectrometry methods used to determine the initial 10 Be/ 9 Be ratio in meteoritic inclusions. Based on analyses of synthesised matrix-matched glass reference materials, we show that the effects of differing major element bulk compositions on the secondary ion yields of Be and B are minor for relevant phases. We demonstrate the importance of using the mean square weighted deviation (MSWD) to interpret the significance of the initial 10 Be/ 9 Be value. For thirty-two CAIs, we recalculated the regressions using literature data, finding that several have unacceptably high MSWD. We calculate the effects of possible sources of isotopic disturbance. Finally, we outline best practices for reporting 10 Be-10 B data, to enable a more refined determination of the initial 10 Be/ 9 Be ratio in the early Solar System.

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“…Gounelle et al, 2006;Gaches et al, 2020). However, several challenges are present in this explanation, including insufficient available energy to produce the whole 26 Al inventory in the disks (Duprat & Tatischeff, 2007), as well as possible inconsistencies with the production of 10 Be, another short-lived radioactive isotope present in the early solar system, which is efficiently produced via spallation (e.g., Jacquet, 2019).…”

Section: The Origin Of the Solar Systemmentioning

confidence: 99%

The Radioactive Nuclei $^{\textbf{26}}$Al and $^{\textbf{60}}$Fe in the Cosmos and in the Solar System

Diehl,

Lugaro,

Heger

et al. 2021

Preprint

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The cosmic evolution of the chemical elements from the Big Bang to the present time is driven by nuclear fusion reactions inside stars and stellar explosions. A cycle of matter recurrently re-processes metal-enriched stellar ejecta into the next generation of stars. The study of cosmic nucleosynthesis and of this matter cycle requires the understanding of the physics of nuclear reactions, of the conditions at which the nuclear reactions are activated inside the stars and stellar explosions, of the stellar ejection mechanisms through winds and explosions, and of the transport of the ejecta towards the next cycle, from hot plasma to cold, star-forming gas. Due to the long timescales of stellar evolution, and because of the infrequent occurrence of stellar explosions, observational studies are challenging, as they have biases in time and space as well as different sensitivities related to the various astronomical methods. Here, we describe in detail the astrophysical and nuclear-physical processes involved in creating two radioactive isotopes useful in such studies, 26 Al and 60 Fe. Due to their radioactive lifetime of the order of a million years these isotopes are suitable to characterise simultaneously the processes of nuclear fusion reactions and of interstellar transport. We describe and discuss the nuclear reactions involved in the production and destruction of 26 Al and 60 Fe, the key characteristics of the stellar sites of their nucleosynthesis and their interstellar journey after ejection from the nucleosynthesis sites. This allows us to connect the theoretical astrophysical aspects to the variety of astronomical messengers presented here, from stardust and cosmic-ray composition measurements, through observation of γ rays produced by radioactivity, to material deposited in deep-sea ocean crusts and to the inferred composition of the first solids that have formed in the Solar System. We show that considering measurements of the isotopic ratio of 26 Al to 60 Fe eliminate some of the unknowns when interpreting astronomical results, and discuss the lessons learned from these two isotopes on cosmic chemical evolution. This review paper has emerged from an ISSI-BJ Team project in 2017-2019, bringing together nuclear physicists, astronomers, and astrophysicists in this inter-disciplinary discussion.

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Beryllium-10 production in gaseous protoplanetary disks and implications for the astrophysical setting of refractory inclusions

Cited by 22 publications

References 83 publications

Fingerprints of the Protosolar Cloud Collapse in the Solar System. II. Nucleosynthetic Anomalies in Meteorites

Fingerprints of the Protosolar Cloud Collapse in the Solar System. II. Nucleosynthetic Anomalies in Meteorites

Best Practices for Determination of Initial ¹⁰Be/⁹Be in Early Solar System Materials by Secondary Ion Mass Spectrometry

The Radioactive Nuclei $^{\textbf{26}}$Al and $^{\textbf{60}}$Fe in the Cosmos and in the Solar System

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Beryllium-10 production in gaseous protoplanetary disks and implications for the astrophysical setting of refractory inclusions

Cited by 22 publications

References 83 publications

Fingerprints of the Protosolar Cloud Collapse in the Solar System. II. Nucleosynthetic Anomalies in Meteorites

Fingerprints of the Protosolar Cloud Collapse in the Solar System. II. Nucleosynthetic Anomalies in Meteorites

Best Practices for Determination of Initial 10Be/9Be in Early Solar System Materials by Secondary Ion Mass Spectrometry

The Radioactive Nuclei $^{\textbf{26}}$Al and $^{\textbf{60}}$Fe in the Cosmos and in the Solar System

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Product

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Best Practices for Determination of Initial ¹⁰Be/⁹Be in Early Solar System Materials by Secondary Ion Mass Spectrometry