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Meyer, B. S.; Clayton, Donald D.

doi:10.1023/a:1005282825778

Cited by 160 publications

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“…Understanding their origin has long been a major goal of cosmochemistry (Russell et al 2001), as it is essential for constraining the stellar environment of the Sun at its birth (Meyer & Clayton 2000), as well as for establishing a chronology of the solar system's first million years (McKeegan & Davis 2005).…”

Section: Introductionmentioning

confidence: 99%

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

Gounelle

Meynet

2012

A&A

128

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: Introductionmentioning

confidence: 99%

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

Gounelle

Meynet

2012

A&A

128

169

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“…Inheritance from the interstellar medium (ISM ) can be ruled out: the average abundance of 60 Fe maintained by ongoing Galactic nucleosynthesis in supernovae and asymptotic giant branch (AGB) stars is estimated at 60 Fe/ 56 Fe = 3 ; 10 À8 (Wasserburg et al 1998) to 60 Fe/ 56 Fe = 3 ; 10 À7 ( Harper 1996), lower than the meteoritic ratio. Moreover, this 60 Fe is injected into the hot phase of the ISM (Meyer & Clayton 2000), and incorporation into molecular clouds and solar systems takes $10 7 yr or more (Meyer & Clayton 2000;Jacobsen 2005), by which time the 60 Fe will have decayed. A late source is argued for (Jacobsen 2005; see also Harper 1996;Meyer & Clayton 2000).…”

Section: Introductionmentioning

confidence: 99%

“…Moreover, this 60 Fe is injected into the hot phase of the ISM (Meyer & Clayton 2000), and incorporation into molecular clouds and solar systems takes $10 7 yr or more (Meyer & Clayton 2000;Jacobsen 2005), by which time the 60 Fe will have decayed. A late source is argued for (Jacobsen 2005; see also Harper 1996;Meyer & Clayton 2000). Production within the solar system itself by irradiation of rocky material by solar energetic particles has been proposed for the origin of other SLRs (e.g., Lee et al 1998;Gounelle et al 2001), but neutron-rich 60 Fe is produced in very low yields by this process.…”

Section: Introductionmentioning

confidence: 99%

Interaction of Supernova Ejecta with Nearby Protoplanetary Disks

Ouellette

Desch

Hester

2007

ApJ

141

229

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The early solar system contained short-lived radionuclides such as 60 Fe (t 1/2 = 1.5 Myr) whose most likely source was a nearby supernova. Previous models of solar system formation considered a supernova shock that triggered the collapse of the Sun's nascent molecular cloud. We advocate an alternative hypothesis, that the solar system's protoplanetary disk had already formed when a very close (<1 pc) supernova injected radioactive material directly into the disk. We conduct the first numerical simulations designed to answer two questions related to this hypothesis: Will the disk be destroyed by such a close supernova, and will any of the ejecta be mixed into the disk? Our simulations demonstrate that the disk does not absorb enough momentum from the shock to escape the protostar to which it is bound. Only low amounts (<1%) of mass loss occur, due to stripping by Kelvin-Helmholtz instabilities across the top of the disk, which also mix into the disk about 1% of the intercepted ejecta. These low efficiencies of destruction and injection are due to the fact that the high disk pressures prevent the ejecta from penetrating far into the disk before stalling. Injection of gas-phase ejecta is too inefficient to be consistent with the abundances of radionuclides inferred from meteorites. On the other hand, the radionuclides found in meteorites would have condensed into dust grains in the supernova ejecta, and we argue that such grains will be injected directly into the disk with nearly 100% efficiency. The meteoritic abundances of the short-lived radionuclides such as 60 Fe therefore are consistent with injection of grains condensed from the ejecta of a nearby (<1 pc) supernova, into an already formed protoplanetary disk.

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“…In this context, 60 Fe (t 1/2 = 2.62 Ma) is particularly important because it can only be synthesized efficiently by stellar nucleosynthesis (Tur et al 2010;Limongi & Chieffi 2006;Timmes et al 1995). Its presence in meteorites hence would provide unambiguous evidence for the arrival of debris from either a supernova explosion or an asymptotic giant branch (AGB) star in the neighborhood of the nascent Sun 15 Ma or less before its formation (Cameron & Truran 1977;Meyer & Clayton 1999;Wasserburg et al 2006). The explosion of a supernova could have been the very event that triggered the formation of the solar system (Cameron & Truran 1977;Vanhala & Boss 2000).…”

Section: Introductionmentioning

confidence: 99%

THE ELUSIVE⁶⁰Fe IN THE SOLAR NEBULA

Moynier

Blichert‐Toft

Wang

et al. 2011

ApJ

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No 60 Ni or 61 Ni anomalies have been detected in troilite inclusions from Muonionalusta, a 4565.3 ± 0.1 Ma old IVA iron meteorite, to the level of the analytical precision of 10 ppm. Because Muonionalusta troilite is very old, has a high Fe/Ni ratio, and is free of 61 Ni anomalies, it is the ideal material in which to search for potential excesses of 60 Ni produced by the decay of 60 Fe (t 1/2 = 2.62 Ma). The 60 Ni/ 58 Ni and Fe/Ni ratios (up to 1680) measured here imply an upper limit for the initial 60 Fe/ 56 Fe for the Muonionalusta troilite of 3 × 10 −9 . Assuming that 60 Fe was homogeneously distributed across the nebula, this result suggests that the solar system initial 60 Fe/ 56 Fe ratio was less than 5 × 10 −9 , which is lower than previously measured by at least a factor of 50.

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Cited by 160 publications

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

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

Interaction of Supernova Ejecta with Nearby Protoplanetary Disks

THE ELUSIVE⁶⁰Fe IN THE SOLAR NEBULA

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Cited by 160 publications

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

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

Interaction of Supernova Ejecta with Nearby Protoplanetary Disks

THE ELUSIVE60Fe IN THE SOLAR NEBULA

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THE ELUSIVE⁶⁰Fe IN THE SOLAR NEBULA