Genetics, crystallization sequence, and age of the South Byron Trio iron meteorites: New insights to carbonaceous chondrite (CC) type parent bodies

Hilton, Connor D.; Bermingham, K. R.; Walker, Richard J.; McCoy, Timothy J.

doi:10.1016/j.gca.2019.02.035

Cited by 34 publications

(25 citation statements)

References 52 publications

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“…2011; Hilton et al. 2019). To do this, we use the parameterization method discussed by Chabot et al.…”

Section: Discussionmentioning

confidence: 99%

“…For magmatic iron meteorite groups, fractional crystallization models of the cores from which they derive may be constrained by identifying at least two iron meteorites that formed as equilibrium solids from the same fractional crystallization sequence (e.g., Hilton et al. 2019). This is not possible for the IIF iron meteorites, however, indicating that a single fractional crystallization model cannot presently be constrained.…”

Section: Discussionmentioning

confidence: 99%

“…Chemical and isotopic similarities have also been noted for the ungrouped Milton pallasite and the South Byron Trio (SBT) iron meteorites, although it is problematic to relate Milton chemically to the SBT core without mixing with metal from a secondary source (Hilton et al. 2019; McCoy et al. 2019).…”

Section: Introductionmentioning

confidence: 99%

“…However, differences in the measured cooling rates of PMG metal (2.5-18 K Myr À1 ) and IIIAB irons (50-350 K Myr À1 ) are difficult to explain in a common core scenario, and have been interpreted by some to suggest that the PMG and IIIAB irons ultimately formed on separate bodies (Yang et al 2010). Chemical and isotopic similarities have also been noted for the ungrouped Milton pallasite and the South Byron Trio (SBT) iron meteorites, although it is problematic to relate Milton chemically to the SBT core without mixing with metal from a secondary source (Hilton et al 2019;McCoy et al 2019).…”

Section: Introductionmentioning

confidence: 99%

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Crystallization histories of the group IIF iron meteorites and Eagle Station pallasites

Hilton

Ash

Walker

2020

Meteorit & Planetary Scien

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The group IIF iron meteorites and Eagle Station pallasites (PES) have highly siderophile element abundances (HSE; Re, Os, Ir, Ru, Pt, and Pd) of metal that are consistent with formation in planetesimal cores by fractional crystallization with minor to major solid metal-liquid metal mixing. Modeling of HSE abundances of the IIF irons indicates a complex formation history that included the mixing of primitive and evolved solid and liquid metals. By contrast, modeling of HSE abundances of PES metal suggests these meteorites formed mainly as equilibrium solids from a common liquid. Abundances of some of the siderophile elements in the IIF irons and PES are permissive of a common core origin; however, the abundances of W and Ni indicate the PES ultimately formed on a more oxidized body. The PES most likely formed by the injection of olivine present at the core-mantle boundary into a metallic core liquid as a result of impact. The core then crystallized inward, trapping the olivine.

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“…2011; Hilton et al. 2019). To do this, we use the parameterization method discussed by Chabot et al.…”

Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Crystallization histories of the group IIF iron meteorites and Eagle Station pallasites

Hilton

Ash

Walker

2020

Meteorit & Planetary Scien

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“…The inner solar system (circa inside of 4 to 5 AU), the domain of the terrestrial planets and rocky asteroids, has been characterized as home to the NC meteorites, the noncarbonaceous meteorites (Warren, 2011). Recent findings from various isotope studies of iron meteorites (Hilton et al., 2019; Kruijer et al., 2014, 2017) show that many of these “NC” bodies formed contemporaneously with and up to 1 Ma after t CAI formation (Hilton et al., 2019). The CC iron meteorites, those relating to carbonaceous chondrites, appear to have formed slightly later (0.5 to 1 Ma) and further out, beyond 4 AU (Hilton et al., 2019; Kruijer et al., 2017).…”

Section: Secular Variation In the Heat And Luminosity Of The Earthmentioning

confidence: 99%

Radiogenic Power and Geoneutrino Luminosity of the Earth and Other Terrestrial Bodies Through Time

McDonough

Šrámek

Wipperfurth

2020

Geochem Geophys Geosyst

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We report the Earth's rate of radiogenic heat production and (anti)neutrino luminosity from geologically relevant short‐lived radionuclides (SLR) and long‐lived radionuclides (LLR) using decay constants from the geological community, updated nuclear physics parameters, and calculations of the β spectra. We track the time evolution of the radiogenic power and luminosity of the Earth over the last 4.57 billion years, assuming an absolute abundance for the refractory elements in the silicate Earth and key volatile/refractory element ratios (e.g., Fe/Al, K/U, and Rb/Sr) to set the abundance levels for the moderately volatile elements. The relevant decays for the present‐day heat production in the Earth (19.9 ± 3.0 TW) are from 40K, 87Rb, 147Sm, 232Th, 235U, and 238U. Given element concentrations in kg‐element/kg‐rock and density ρ in kg/m3, a simplified equation to calculate the present‐day heat production in a rock is h[μW m−3]=ρ3.387×10−3K+0.01139Rb+0.04595Sm+26.18Th+98.29U The radiogenic heating rate of Earth‐like material at solar system formation was some 103 to 104 times greater than present‐day values, largely due to decay of 26Al in the silicate fraction, which was the dominant radiogenic heat source for the first ∼10 Ma. Assuming instantaneous Earth formation, the upper bound on radiogenic energy supplied by the most powerful short‐lived radionuclide 26Al (t1/2 = 0.7 Ma) is 5.5×1031 J, which is comparable (within a factor of a few) to the planet's gravitational binding energy.

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Radiogenic power and geoneutrino luminosity of the Earth and other terrestrial bodies through time

McDonough

Šrámek

Wipperfurth

2019

Preprint

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Key Points:• Radiogenic heat production and geoneutrino luminosity calculated over the age of the Earth • Simple formulae proposed for evaluation at arbitrary planetary composition • Differences in radioactive decay parameters highlighted between nuclear physics and geological communities AbstractWe report the Earth's rate of radiogenic heat production and (anti)neutrino luminosity from geologically relevant short-lived radionuclides (SLR) and long-lived radionuclides (LLR) using decay constants from the geological community, updated nuclear physics parameters, and calculations of the β spectra. We carefully account for all branches in 40 K decay using the updated β − energy spectrum from physics and an updated branching ratio from geological studies. We track the time evolution of the radiogenic power and luminosity of the Earth over the last 4.57 billion years, assuming an absolute abundance for the refractory elements in the silicate Earth and key volatile/refractory element ratios (e.g., Fe/Al, K/U, and Rb/Sr) to set the abundance levels for the moderately volatile elements. The relevant decays for the present-day heat production in the Earth (19.9 ± 3.0 TW) are from 40 K, 87 Rb, 147 Sm, 232 Th, 235 U, and 238 U. Given element concentrations in kg-element/kg-rock and density ρ in kg/m 3 , a simplified equation to calculate the heat production in a rock is:3.387 × 10 −3 [K] + 0.01139 [Rb] + 0.04607 [Sm] + 26.18 [Th] + 98.29 [U]The radiogenic heating rate of earth-like material at Solar System formation was some 10 3 to 10 4 times greater than present-day values, largely due to decay of 26 Al in the silicate fraction, which was the dominant radiogenic heat source for the first ∼ 10 My. Decay of 60 Fe contributed a non-negligible amount of heating during the first ∼ 15 My after CAI (Calcium Aluminum Inclusion) formation, interestingly within the time frame of core-mantle segregation. Using factors and equations presented here, one can calculate the first-order thermal and (anti)neutrino luminosity history of various size bodies in the solar system and exoplanets. Plain Language SummaryThe decay of radioactive elements in planetary interior's produces heat that drives the dynamic processes of convection (core and mantle), melting and volcanism in rocky bodies in the solar system and beyond. For elements with half-lives of 100,000 to 100 billion years, uncertainties in their decay constants range from 0.2% to ∼ 4% absolute and about 1% to 4% relative when comparing data sources in physics and geology. These differences, combined with uncertainties in Q (heat of reaction) values, lead to diverging results for heat production and for predictions of the amount of energy removed from the rocky body by emitted (anti)neutrinos.

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Genetics, crystallization sequence, and age of the South Byron Trio iron meteorites: New insights to carbonaceous chondrite (CC) type parent bodies

Cited by 34 publications

References 52 publications

Crystallization histories of the group IIF iron meteorites and Eagle Station pallasites

Crystallization histories of the group IIF iron meteorites and Eagle Station pallasites

Radiogenic Power and Geoneutrino Luminosity of the Earth and Other Terrestrial Bodies Through Time

Radiogenic power and geoneutrino luminosity of the Earth and other terrestrial bodies through time

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