2017
DOI: 10.3847/1538-4357/aa992e
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Triggered Star Formation inside the Shell of a Wolf–Rayet Bubble as the Origin of the Solar System

Abstract: A critical constraint on solar system formation is the high 26 Al/ 27 Al abundance ratio of 5 × 10 −5 at the time of formation, which was about 17 times higher than the average Galactic ratio, while the 60 Fe/ 56 Fe value was about 2 × 10 −8 , lower than the Galactic value. This challenges the assumption that a nearby supernova (SN) was responsible for the injection of these short-lived radionuclides into the early solar system. We show that this conundrum can be resolved if the solar system was formed by a tr… Show more

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Cited by 59 publications
(77 citation statements)
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“…The stellar contribution of 26 Al (and probably 41 Ca) to ESS in the proposed scenario would require the role of an independent Wolf-Rayet wind (Sahijpal & Soni 2006;Dwarkadas et al 2017) without any trailed 60 Fe rich supernova contribution. Sahijpal & Soni (2006) Finally, in order to understand the influence of the prolonged star formation within a single stellar cluster on the SLRs yields we have performed simulations (Models CI and DI) with distinct star formation histories (Table 1).…”
Section: Discussionmentioning
confidence: 95%
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“…The stellar contribution of 26 Al (and probably 41 Ca) to ESS in the proposed scenario would require the role of an independent Wolf-Rayet wind (Sahijpal & Soni 2006;Dwarkadas et al 2017) without any trailed 60 Fe rich supernova contribution. Sahijpal & Soni (2006) Finally, in order to understand the influence of the prolonged star formation within a single stellar cluster on the SLRs yields we have performed simulations (Models CI and DI) with distinct star formation histories (Table 1).…”
Section: Discussionmentioning
confidence: 95%
“…3c indicates the approximate match with the initial 53 Mn/ 55 Mn and 60 Fe/ 56 Fe values in the ESS at the time of the formation of CAIs. This could explain three possible ways for the contribution of the two radionuclides, 53 Mn and 60 Fe, from already evolved stellar clusters to the presolar cloud, with an independent contribution of 26 Al (and 41 Ca) from a Wolf-Rayet star (Sahijpal & Soni 2006;Dwarkadas et al 2017). € The SLR stellar yields of the core-collapse supernovae were only considered for Heter-Models…”
Section: Acknowledgementsmentioning
confidence: 99%
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“…The ratio of 60 Fe / 26 Al excludes an origin from a nearby core-collapse supernova explosion because this would result in a very low (Ouellette et al 2010) but comparable abundances in 26 Al as well as in 60 Fe (Nomoto et al 2006). An even earlier enrichment of the pre-solar nebula by the wind of a 1.6 to 6 M asymptotic giant-branch star (Mowlavi & Meynet 2000;Wasserburg et al 2006) is hard to reconcile with the timescales of star formation and disk evolution (Isella et al 2009), and an early pre-solar enrichment through a > ∼ 20 M Wolf-Rayet star (Dearborn & Blake 1988;Gaidos et al 2009;Tatischeff et al 2010;Gounelle & Meynet 2012;Dwarkadas et al 2017) and its subsequent supernova would lead to an anomalously high abundance in 60 Fe . These scenarios have difficulty explaining the Send offprint requests to: S. Portegies Zwart observed SLRs and neither of these explains the outer edge of the solar system's planetesimal disk, its tilt with respect to the Sun's equatorial plane or the high temperatures needed for producing vitreous droplets in chondrules.…”
Section: Introductionmentioning
confidence: 99%