Timing of Nebula Processes That Shaped the Precursors of the Terrestrial Planets

Chaussidon, M.; Liu, Ming‐Chang

doi:10.1002/9781118860359.ch1

Cited by 4 publications

(3 citation statements)

References 199 publications

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“…In our model, collisions of chondrule-eligible planetesimals preferentially produced a chondrule formation peak at around t ∼ 2 Myr after CAIs (Figure 8 and Supplementary Figures). Although the exact timing depends on the parameter choice, this peak is in very good agreement with the radiogenic ages determined for chondrules in meteorites (Villeneuve et al, 2009;Mishra and Chaussidon, 2014;Chaussidon and Liu, 2015, see chondrule geochronology Section 4.4). In our models, the peak reflects the temperature climax of planetesimals heated from 26 Al decay (as suggested in Sanders and Scott, 2012).…”

Section: Accretion and Dynamical Recyclingsupporting

confidence: 79%

“…(i) A homogeneous 26 Al distribution entails that precise Al-Mg ages of chondrules can be obtained and these indicate a time gap of ∆t = 0.5-1.0 Myr between the formation of CAIs (at t ∼ 0 Myr) and the onset of chondrule formation (Villeneuve et al, 2009;Kita and Ushikubo, 2012;Nagashima et al, 2014;Chaussidon and Liu, 2015;Villeneuve et al, 2015). In Section 4.2 we argued that the apparent peak in chondrule formation ages may be linked to the interior heat climax of 26 Al-heated planetesimals.…”

Section: Chondrule Geochronologymentioning

confidence: 97%

“…Based on various radiometric dating techniques, chondrules formed during the first ∼ 4-6 Myr after CAIs (Scott and Krot, 2014;Chaussidon and Liu, 2015). The exact details, however, are debated.…”

Section: Chondrule Geochronologymentioning

confidence: 99%

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Impact splash chondrule formation during planetesimal recycling

Lichtenberg

Golabek

Dullemond

et al. 2018

Icarus

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Chondrules, mm-sized igneous-textured spherules, are the dominant bulk silicate constituent of chondritic meteorites and originate from highly energetic, local processes during the first million years after the birth of the Sun. So far, an astrophysically consistent chondrule formation scenario explaining major chemical, isotopic and textural features, in particular Fe,Ni metal abundances, bulk Fe/Mg ratios and intra-chondrite chemical and isotopic diversity, remains elusive. Here, we examine the prospect of forming chondrules from impact splashes among planetesimals heated by radioactive decay of short-lived radionuclides using thermomechanical models of their interior evolution. We show that intensely melted planetesimals with interior magma oceans became rapidly chemically equilibrated and physically differentiated. Therefore, collisional interactions among such bodies would have resulted in chondrule-like but basaltic spherules, which are not observed in the meteoritic record. This inconsistency with the expected dynamical interactions hints at an incomplete understanding of the planetary growth regime during the lifetime of the solar protoplanetary disk. To resolve this conundrum, we examine how the observed chemical and isotopic features of chondrules constrain the dynamical environment of accreting chondrite parent bodies by interpreting the meteoritic record as an impact-generated proxy of early solar system planetesimals that underwent repeated collision and reaccretion cycles. Using a coupled evolution-collision model we demonstrate that the vast majority of collisional debris feeding the asteroid main belt must be derived from planetesimals which were partially molten at maximum. Therefore, the precursors of chondrite parent bodies either formed primarily small, from sub-canonical aluminum-26 reservoirs, or collisional destruction mechanisms were efficient enough to shatter planetesimals before they reached the magma ocean phase. Finally, we outline the window in parameter space for which chondrule formation from planetesimal collisions can be reconciled with the meteoritic record and how our results can be used to further constrain early solar system dynamics.

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Section: Accretion and Dynamical Recyclingsupporting

confidence: 79%

Section: Chondrule Geochronologymentioning

confidence: 97%

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Impact splash chondrule formation during planetesimal recycling

Lichtenberg

Golabek

Dullemond

et al. 2018

Icarus

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Irradiation origin of 10Be in the solar nebula: Evidence from Li-Be-B and Al-Mg isotope systematics, and REE abundances of CAIs from Yamato-81020 CO3.05 chondrite

Fukuda

Hiyagon

Fujiya

et al. 2021

Geochimica et Cosmochimica Acta

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Lifetime of the solar nebula constrained by meteorite paleomagnetism

Wang

Weiss

Bai

et al. 2017

Science

188

161

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A key stage in planet formation is the evolution of a gaseous and magnetized solar nebula. However, the lifetime of the nebular magnetic field and nebula are poorly constrained. We present paleomagnetic analyses of volcanic angrites demonstrating that they formed in a near-zero magnetic field (<0.6 microtesla) at 4563.5 ± 0.1 million years ago, ~3.8 million years after solar system formation. This indicates that the solar nebula field, and likely the nebular gas, had dispersed by this time. This sets the time scale for formation of the gas giants and planet migration. Furthermore, it supports formation of chondrules after 4563.5 million years ago by non-nebular processes like planetesimal collisions. The core dynamo on the angrite parent body did not initiate until about 4 to 11 million years after solar system formation.

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Timing of Nebula Processes That Shaped the Precursors of the Terrestrial Planets

Cited by 4 publications

References 199 publications

Impact splash chondrule formation during planetesimal recycling

Impact splash chondrule formation during planetesimal recycling

Irradiation origin of 10Be in the solar nebula: Evidence from Li-Be-B and Al-Mg isotope systematics, and REE abundances of CAIs from Yamato-81020 CO3.05 chondrite

Lifetime of the solar nebula constrained by meteorite paleomagnetism

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