Terrestrial planet formation from lost inner solar system material

Burkhardt, C.; Spitzer, Fridolin; Morbidelli, Alessandro; Budde, G.; Render, Jan; Kruijer, T. S.; Kleine, T.

doi:10.1126/sciadv.abj7601

Cited by 80 publications

(63 citation statements)

References 64 publications

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“…The resulting diffusion and depletion timescales of volatiles then depend on the thickness of the bulk water ice that needs to be passed, and on the sizes of the icy pebbles accordingly. Further, uncertainties are caused by possible migration processes within the solar nebula and the protoplanetary disc [ 5 , 74 , 75 ], as reservoirs of pebbles from different regions further outside the solar nebula could contribute to the volatile content in the forming carbonaceous chondrite parent bodies.…”

Section: Methodsmentioning

confidence: 99%

Possible Ribose Synthesis in Carbonaceous Planetesimals

Paschek

Köhler

Pearce

et al. 2022

Life

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The origin of life might be sparked by the polymerization of the first RNA molecules in Darwinian ponds during wet-dry cycles. The key life-building block ribose was found in carbonaceous chondrites. Its exogenous delivery onto the Hadean Earth could be a crucial step toward the emergence of the RNA world. Here, we investigate the formation of ribose through a simplified version of the formose reaction inside carbonaceous chondrite parent bodies. Following up on our previous studies regarding nucleobases with the same coupled physico-chemical model, we calculate the abundance of ribose within planetesimals of different sizes and heating histories. We perform laboratory experiments using catalysts present in carbonaceous chondrites to infer the yield of ribose among all pentoses (5Cs) forming during the formose reaction. These laboratory yields are used to tune our theoretical model that can only predict the total abundance of 5Cs. We found that the calculated abundances of ribose were similar to the ones measured in carbonaceous chondrites. We discuss the possibilities of chemical decomposition and preservation of ribose and derived constraints on time and location in planetesimals. In conclusion, the aqueous formose reaction might produce most of the ribose in carbonaceous chondrites. Together with our previous studies on nucleobases, we found that life-building blocks of the RNA world could be synthesized inside parent bodies and later delivered onto the early Earth.

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Section: Methodsmentioning

confidence: 99%

Possible Ribose Synthesis in Carbonaceous Planetesimals

Paschek

Köhler

Pearce

et al. 2022

Life

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“…We note that current work on Earth's isotopic composition suggests that Earth is a mixture from different regions of the disk, rather than sourcing material from a single location (e.g. Fischer-Gödde et al 2020;Burkhardt et al 2021) The HSE Ruthenium has been the subject of several recent studies (e.g. Dauphas 2017;Bermingham et al 2018;Fischer-Gödde et al 2020).…”

Section: Late Accretionmentioning

confidence: 94%

“…Molybdenum, on the other hand, is moderately siderophile; while the early-delivered Mo is expected to have partitioned into the growing core, Mo delivered during the later stages of accretion would leave a signature in the mantle. Mo isotopes, therefore, trace the accretion of the final ∼10% of Earth's mass (Dauphas 2017;Burkhardt et al 2021). Meteorites reveal that the isotopic compositions of Mo and Ru are correlated (e.g.…”

Section: Late Accretionmentioning

confidence: 99%

Did Earth eat its leftovers? Impact ejecta as a component of the late veneer

Carter¹,

Stewart²

2022

Preprint

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The presence of highly siderophile elements in Earth's mantle indicates that a small percentage of Earth's mass was delivered after the last giant impact in a stage of 'late accretion.' There is ongoing debate about the nature of late-accreted material and the sizes of late-accreted bodies. Earth appears isotopically most similar to enstatite chondrites and achondrites. It has been suggested that late accretion must have been dominated by enstatite-like bodies that originated in the inner disk, rather than ordinary or carbonaceous chondrites. Here, we examine the provenances of 'leftover' planetesimals present in the inner disk in the late stages of accretion simulations. Dynamically excited planet formation produces planets and embryos with similar provenances, suggesting that the Moon-forming impactor may have had a stable isotope composition very similar to the proto-Earth. Commonly, some planetesimal-sized bodies with similar provenances to the Earth-like planets are left at the end of the main stage of growth. The most chemically-similar planetesimals are typically fragments of proto-planets ejected millions of years earlier. If these similar-provenance bodies are later accreted by the planet, they will represent late-accreted mass that naturally matches Earth's composition. The planetesimal-sized bodies that exist during the giant impact phase can have large core mass fractions, with core provenances similar to the proto-Earth. These bodies are an important potential source for highly siderophile elements. The range of core fractions in leftover planetesimals complicates simple inferences as to the mass and origin of late accretion based on the highly siderophile elements in the mantle.

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“…the meteorite collection) such an unbiased sample does not exist (Mezger et al 2020;Burkhardt et al 2021). For exoplanetary systems the task is even harder.…”

Section: Polluted White Dwarf Constraints On Core-mantle Differentiationmentioning

confidence: 99%

Prevalence of short-lived radioactive isotopes across exoplanetary systems inferred from polluted white dwarfs

Curry,

Bonsor,

Lichtenberg

et al. 2022

Preprint

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In the Solar System short-lived radioisotopes, such as 26 Al, played a crucial role during the formation planetary bodies by providing a significant additional source of heat. Notably, this led to early and large-scale melting and iron core formation in planetesimals and their loss of volatile elements, such as hydrogen and carbon. In the context of exoplanetary systems, therefore, the prevalence of short-lived radioisotopes is key to interpreting the observed bulk volatile budget and atmospheric diversity among low-mass exoplanets. White dwarfs that have accreted planetary material provide a unique means to infer the frequency of iron core formation in extrasolar planetesimals, and hence the ubiquity of planetary systems forming with high short-lived radioisotope abundances. Here, we devise a quantitative method to infer the fraction of planetary systems enriched with shortlived radionuclides upon planetesimal formation from white dwarf data. We argue that the current evidence from white dwarfs point towards a significant fraction of exo-planetesimals having formed an iron core. Although the data may be explained by the accretion of exo-moon or Pluto-sized bodies that were able to differentiate due to gravitational potential energy release, our results suggest that the most likely explanation for the prevalence of differentiated material among polluted white dwarfs is that the Solar System is not unusual in being enriched in 26 Al. The models presented here suggest a ubiquitous pathway for the enrichment of exoplanetary systems by short-lived radioisotopes, disfavouring short-lived radioisotope enrichment scenarios relying on statistically rare chance encounters with single nearby supernovae, Wolf-Rayet or AGB stars.

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Terrestrial planet formation from lost inner solar system material

Abstract: An integrated assessment of isotopic variations among meteorites reveals the process by which Earth and Mars are formed.

Cited by 80 publications

References 64 publications

Possible Ribose Synthesis in Carbonaceous Planetesimals

Possible Ribose Synthesis in Carbonaceous Planetesimals

Did Earth eat its leftovers? Impact ejecta as a component of the late veneer

Prevalence of short-lived radioactive isotopes across exoplanetary systems inferred from polluted white dwarfs

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