THE ELUSIVE<sup>60</sup>Fe IN THE SOLAR NEBULA

Moynier, Frédéric; Blichert‐Toft, Janne; Wang, Kun; Herzog, G. F.; Albarède, F.

doi:10.1088/0004-637x/741/2/71

Cited by 29 publications

(19 citation statements)

References 66 publications

(79 reference statements)

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“…Recent evidence has raised doubts about the initial amount of 60 Fe present in the solar nebula. Moynier et al (2011) presented evidence for an initial ratio of 60 Fe/ 56 Fe less than 3 × 10 −9 , roughly 100 times smaller than previously published ratios (e.g., Mishra et al 2010), while Tang & Dauphas (2012) found an initial ratio of 1 × 10 −8 . The initial level of 60 Fe is particularly significant, as its efficient production requires stellar nucleosynthesis (Tachibana et al 2006) in either a massive star supernova or an AGB star (Huss et al 2009).…”

Section: Introductioncontrasting

confidence: 47%

“…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%

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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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Section: Introductioncontrasting

confidence: 47%

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 first generation cluster with N 1 = 5000 stars and γ SN = 0.02 is a possible reasonable solution. If, as recently suggested (Moynier et al 2011), the solar system initial abundance of 60 Fe was lower than the one usually accepted, γ SN or N 1 could accordingly be decreased.…”

Section: Constraining Generation #1: the Grandparent Cluster Sizementioning

confidence: 83%

“…As in any family, the further back in time one goes, the more difficult it is to retrieve precise information on ancestors. More knowledge will be gained on N 1 when analysts have converged on the initial solar system value of 60 Fe (Quitté et al 2010;Moynier et al 2011), along with the development of numerical simulations that will help to better constrain the value of γ SN .…”

Section: Discussionmentioning

confidence: 99%

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

Gounelle

Meynet

2012

A&A

130

173

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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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“…Telus et al (2012) and Ogliore et al (2011), however, demonstrated that these high ratios were due to improper data reduction. Using another instrumental approach based on the analysis of bulk chondrites and differentiated meteorites, a diversity of groups have suggested that the initial solar system 60 Fe/ 56 Fe ratio was two orders of magnitude lower than previously thought, with an upper limit of 1 × 10 −8 (Tang & Dauphas 2012;Moynier et al 2011;Quitté et al 2011). Very few chondrules still show higher initial ratios (Mishra & Chaussidon 2014), possibly because of nickel redistribution on the mineral scale (Chaussidon & Barrat 2009) 60 Fe has been positively detected in very few objects, if any, this short-lived radionuclide seems to have been homogeneously distributed in the SPD (Tang & Dauphas 2012).…”

Section: Experimental Datamentioning

confidence: 98%

The abundance of²⁶Al-rich planetary systems in the Galaxy

Gounelle

2015

A&A

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One of the most puzzling properties of the solar system is the high abundance at its birth of 26 Al, a short-lived radionuclide with a mean life of 1 Myr. Now decayed, it has left its imprint in primitive meteoritic solids. The origin of 26 Al in the early solar system has been debated for decades and strongly constrains the astrophysical context of the Sun and planets formation. We show that, according to the present understanding of star-formation mechanisms, it is very unlikely that a nearby supernova has delivered 26 Al into the nascent solar system. A more promising model is the one whereby the Sun formed in a wind-enriched, 26 Al-rich dense shell surrounding a massive star (M > 32 M ). We calculate that the probability of any given star in the Galaxy being born in such a setting, corresponding to a well-known mode of star formation, is of the order of 1%. It means that our solar system, though not the rule, is relatively common and that many exo-planetary systems in the Galaxy might exhibit comparable enrichments in 26 Al. Such enrichments played an important role in the early evolution of planets because 26 Al is the main heat source for planetary embryos.

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THE ELUSIVE⁶⁰Fe IN THE SOLAR NEBULA

Cited by 29 publications

References 66 publications

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

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

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

The abundance of²⁶Al-rich planetary systems in the Galaxy

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THE ELUSIVE60Fe IN THE SOLAR NEBULA

Cited by 29 publications

References 66 publications

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

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

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

The abundance of26Al-rich planetary systems in the Galaxy

Contact Info

Product

Resources

About

THE ELUSIVE⁶⁰Fe IN THE SOLAR NEBULA

The abundance of²⁶Al-rich planetary systems in the Galaxy