HETEROGENEOUS DISTRIBUTION OF
                    <sup>26</sup>
                    Al AT THE BIRTH OF THE SOLAR SYSTEM

Makide, K.; Nagashima, K.; Krot, Alexander N.; Huss, G. R.; Ciesla, F. J.; Hellebrand, E.; Gaidos, Eric; Yang, Le

doi:10.1088/2041-8205/733/2/l31

Cited by 92 publications

(98 citation statements)

References 49 publications

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“…Injection takes place on only one side of the dense shell. Because some time will be needed for 26 Al carriers (gas or solid) to diffuse within the shell entire volume, it is expected that the first solids to form close to the protostar, as expected for CAIs ), will not contain 26 Al, as is observed in some meteoritic samples (Liu et al 2009;Makide et al 2011;Weber et al 1995). Though the exact diffusion timescale is difficult to quantify without entering desired complex numerical simulations, it is expected to be close to the crossing time of the core, i.e.…”

Section: Discussionmentioning

confidence: 99%

Solar system genealogy revealed by extinct short-lived radionuclides in meteorites

Gounelle

Meynet

2012

A&A

133

169

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Context. Little is known about the stellar environment and the genealogy of our solar system. Short-lived radionuclides (SLRs, mean lifetime τ shorter than 100 Myr) that were present in the solar protoplanetary disk 4.56 Gyr ago could potentially provide insight into that key aspect of our history, were their origin understood. Aims. Previous models failed to provide a reasonable explanation of the abundance of two key SLRs, 26 Al (τ 26 = 1.1 Myr) and 60 Fe (τ 60 = 3.7 Myr), at the birth of the solar system by requiring unlikely astrophysical conditions. Our aim is to propose a coherent and generic solution based on the most recent understanding of star-forming mechanisms. Methods. Iron-60 in the nascent solar system is shown to have been produced by a diversity of supernovae belonging to a first generation of stars in a giant molecular cloud. Aluminum-26 is delivered into a dense collected shell by a single massive star wind belonging to a second star generation. The Sun formed in the collected shell as part of a third stellar generation. Aluminum-26 yields used in our calculation are based on new rotating stellar models in which 26 Al is present in stellar winds during the star main sequence rather than during the Wolf-Rayet phase alone. Our scenario eventually constrains the time sequence of the formation of the two stellar generations that just preceded the solar system formation, along with the number of stars born in these two generations. Results. We propose a generic explanation for the past presence of SLRs in the nascent solar system, based on a collect-injection-andcollapse mechanism, occurring on a diversity of spatial/temporal scales. In that model, the presence of SLRs with a diversity of mean lifetimes in the solar protoplanetary disk is simply the fossilized record of sequential star formation within a hierarchical interstellar medium. We identify the genealogy of our solar system's three star generations earlier. In particular, we show that our Sun was born together with a few hundred stars in a dense collected shell situated at a distance of 5−10 pc from a parent massive star having a mass greater than about 30 solar masses and belonging to a cluster containing ∼1200 stars.

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Section: Discussionmentioning

confidence: 99%

Solar system genealogy revealed by extinct short-lived radionuclides in meteorites

Gounelle

Meynet

2012

A&A

133

169

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“…Assuming the suitability of our shock front parameters, the 3D models show that a relatively small number of RT fingers are likely to have been involved in the injection of the SNR SLRIs into the solar nebula, which has significant consequences for the processes of mixing and transport that occurred after injection into the nebula (e.g., Boss 2011) and for the resulting levels of isotopic homogeneity and heterogeneity (e.g., Bouvier & Wadhwa 2010;Schiller et al 2010;Larsen et al 2011;Makide et al 2011;Wang et al 2011;Boss 2012). Furthermore, our estimates of injection efficiencies and dilution factors will become important discriminators for judging the likelihood of the supernova triggering and injection scenario once a clearer picture emerges of the initial abundances of the SLRIs (principally 60 Fe: Moynier et al 2011;Telus et al 2012) that were present during the formation of the various components of the most primitive meteorites.…”

Section: Discussionmentioning

confidence: 99%

Supernova-Triggered Molecular Cloud Core Collapse and the Rayleigh-Taylor Fingers That Polluted the Solar Nebula

Boss¹,

Keiser²

2012

ApJ

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A supernova is a likely source of short-lived radioisotopes (SLRIs) that were present during the formation of the earliest solar system solids. A suitably thin and dense supernova shock wave may be capable of triggering the selfgravitational collapse of a molecular cloud core while simultaneously injecting SLRIs. Axisymmetric hydrodynamics models have shown that this injection occurs through a number of Rayleigh-Taylor (RT) rings. Here we use the FLASH adaptive mesh refinement (AMR) hydrodynamics code to calculate the first fully three dimensional (3D) models of the triggering and injection process. The axisymmetric RT rings become RT fingers in 3D. While ∼ 100 RT fingers appear early in the 3D models, only a few RT fingers are likely to impact the densest portion of the collapsing cloud core. These few RT fingers must then be the source of any SLRI spatial heterogeneity in the solar nebula inferred from isotopic analyses of chondritic meteorites. The models show that SLRI injection efficiencies from a supernova several pc away fall at the lower end of the range estimated for matching SLRI abundances, perhaps putting them more into agreement with recent reassessments of the level of 60 Fe present in the solar nebula.

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“…Moreover, the abundance of rare-earth elements and the oxygen isotope composition of FUN CAIs indicate that their precursors formed as condensates from a solar gas (Holst et al 2013). Collectively, these observations are often interpreted as reflecting the formation of FUN CAIs prior to the admixing of stellar-derived 26 Al to the CAI forming gas (Sahijpal & Goswami 1998;Thrane et al 2008;Makide et al 2011;Boss & Keiser 2012, 2013Pan et al 2012). If this interpretation is correct, these objects can be used to track the timing of the addition of 26 Al to the forming protoplanetary disk.…”

Section: Introductionmentioning

confidence: 99%

TRACKING THE DISTRIBUTION OF ²⁶Al AND ⁶⁰Fe DURING THE EARLY PHASES OF STAR AND DISK EVOLUTION

Küffmeier

Mogensen

Haugboelle

et al. 2016

ApJ

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Fe ratios of accreting gas within a vicinity of 1000 au of the stars follow the predicted decay curves of the initial abundances at the time of star formation without evidence of spatial or temporal heterogeneities for the first 100 kyr of star formation. Therefore, the observed differences in 26 Al/ 27 Al ratios between FUN and canonical CAIs are likely not caused by admixing of supernova material during the early evolution of the proto-Sun. Selective thermal processing of dust grains is a more viable scenario to account for the heterogeneity in 26 Al/ 27 Al ratios at the time of solar system formation.

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HETEROGENEOUS DISTRIBUTION OF ²⁶ Al AT THE BIRTH OF THE SOLAR SYSTEM

Abstract: It is believed that 26 Al, a short-lived (t 1/2 = 0.73 Ma) and now extinct radionuclide, was uniformly distributed in the nascent Solar System with the initial 26 Al/ 27 Al ratio of ~5.2×10

Cited by 92 publications

References 49 publications

Solar system genealogy revealed by extinct short-lived radionuclides in meteorites

Solar system genealogy revealed by extinct short-lived radionuclides in meteorites

Supernova-Triggered Molecular Cloud Core Collapse and the Rayleigh-Taylor Fingers That Polluted the Solar Nebula

TRACKING THE DISTRIBUTION OF ²⁶Al AND ⁶⁰Fe DURING THE EARLY PHASES OF STAR AND DISK EVOLUTION

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HETEROGENEOUS DISTRIBUTION OF 26 Al AT THE BIRTH OF THE SOLAR SYSTEM

Abstract: It is believed that 26 Al, a short-lived (t 1/2 = 0.73 Ma) and now extinct radionuclide, was uniformly distributed in the nascent Solar System with the initial 26 Al/ 27 Al ratio of ~5.2×10

Cited by 92 publications

References 49 publications

Solar system genealogy revealed by extinct short-lived radionuclides in meteorites

Solar system genealogy revealed by extinct short-lived radionuclides in meteorites

Supernova-Triggered Molecular Cloud Core Collapse and the Rayleigh-Taylor Fingers That Polluted the Solar Nebula

TRACKING THE DISTRIBUTION OF 26Al AND 60Fe DURING THE EARLY PHASES OF STAR AND DISK EVOLUTION

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HETEROGENEOUS DISTRIBUTION OF ²⁶ Al AT THE BIRTH OF THE SOLAR SYSTEM

TRACKING THE DISTRIBUTION OF ²⁶Al AND ⁶⁰Fe DURING THE EARLY PHASES OF STAR AND DISK EVOLUTION