Fossil records of high level of 60Fe in chondrules from unequilibrated chondrites

Mishra, R. K.; Chaussidon, M.

doi:10.1016/j.epsl.2014.04.032

Cited by 36 publications

(43 citation statements)

References 38 publications

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“…Using that lower ratio, Young (2014Young ( , 2016 argued that there was no need for a recent SN injection, and that the initial abundances of a dozen SLRIs could be explained by the contributions of massive star winds to the general interstellar medium in regions of star formation. However, other studies continued to find high initial 60 Fe/ 56 Fe ratios, now in unequilibrated OC (UOC), of ∼ 7 × 10 −7 , ∼ 2 − 8 × 10 −7 , and ∼ 8 − 11 × 10 −7 , respectively (Mishra & Goswami 2014;Mishra & Chaussidon 2014;Mishra et al 2016). As a result, a mystery arose regarding 60 Fe analyses of individual chondrules compared to bulk samples.…”

Section: Early Estimates Of the Initial Amount Ofmentioning

confidence: 99%

Triggering Collapse of the Presolar Dense Cloud Core and Injecting Short-lived Radioisotopes with a Shock Wave. V. Nonisothermal Collapse Regime

Boss

2017

ApJ

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Recent meteoritical analyses support an initial abundance of the short-lived radioisotope 60 Fe that may be high enough to require nucleosynthesis in a core collapse supernova, followed by rapid incorporation into primitive meteoritical components, rather than a scenario where such isotopes were inherited from a well-mixed region of a giant molecular cloud polluted by a variety of supernovae remnants and massive star winds. This paper continues to explore the former scenario, by calculating three dimensional, adaptive mesh refinement, hydrodynamical code (FLASH 2.5) models of the self-gravitational, dynamical collapse of a molecular cloud core that has been struck by a thin shock front with a speed of 40 km/sec, leading to the injection of shock front matter into the collapsing cloud through the formation of Rayleigh-Taylor fingers at the shock-cloud intersection. These models extend the previous work into the nonisothermal collapse regime using a polytropic approximation to represent compressional heating in the optically thick protostar. The models show that the injection efficiencies of shock front material are enhanced compared to previous models, which were not carried into the nonisothermal regime and so did not reach such high densities. The new models, combined with the recent estimates of initial 60 Fe abundances, imply that the supernova triggering and injection scenario remains as a plausible explanation for the origin of the short-lived radioisotopes involved in the formation of our solar system.

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Section: Early Estimates Of the Initial Amount Ofmentioning

confidence: 99%

Triggering Collapse of the Presolar Dense Cloud Core and Injecting Short-lived Radioisotopes with a Shock Wave. V. Nonisothermal Collapse Regime

Boss

2017

ApJ

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“…Yet subsequent work has continued to report high inferred 60 Fe/ 56 Fe° (see Fig. 6c) from in situ analyses of chondrules in studies for which such statistical bias is argued to be insignificant (Mishra and Goswami, 2014;Mishra and Chaussidon, 2014;Mishra et al, 2016).…”

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confidence: 99%

“…This contrast in conclusions from bulk and in situ approaches also extends to other MC-ICPMS work. Regelous et al (2008) and Steele et al (2012) Mishra and Chaussidon (2014) and respectively. The former inferred 60 Fe/ 56 Fe° (3±2)x10 -7 whereas the latter, as discussed above, argued for (1±3)x10 -9 .…”

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confidence: 99%

“…Even for high resolution SIMS measurements, 59 CoH + overlaps considerably with 60 Ni + (Mishra and Chaussidon, 2014) and depending on measurement mass, it may not be resolved at all. The high Fe/Ni portions of chondrules are the result of fractional removal of olivine and/or low-Ca pyroxene and troilite from the cooling melt droplet.…”

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confidence: 99%

“…7). This is the model value for a ferro-magnesian phase (specifically olivine) grown from the residual melt, as this was the main target in the study of Mishra and Chaussidon (2014) 26 Al of the solar system is to be explained by recent injection of stellar material, this must come from a source which does not also generate significant 60 Fe. Tang and Dauphas (2012) suggest that winds from the outer portions of a giant, Wolf-Rayet star could p11 constitute an appropriate explanation.…”

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confidence: 99%

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