The Effect of Jupiter's Formation on the Distribution of Refractory Elements and Inclusions in Meteorites

Abstract

We present a comprehensive evolutionary model of the Sun's protoplanetary disk, constructed to resolve the "CAI Storage" problem of meteoritics. We predict the abundances of calcium-rich, aluminum-rich inclusions (CAIs) and refractory lithophile elements under the central assumption that Jupiter's ∼ 30 M ⊕ core forms at about 3 AU at around 0.6 Myr and opened a gap CAIs are trapped in the pressure maximum beyond Jupiter; carbonaceous chondrites formed there. Inside Jupiter's orbit, CAIs were depleted by aerodynamic drag; ordinary and enstatite chondrites formed there. For 16 chondrites and achondrites, we review meteoritic data on their CAI and refractory abundances and their times of formation, constrained by radiometric dating and thermal models. We predict their formation locations, finding excellent consistency with other location information (water content, asteroid spectra and parent bodies). We predict the size of particle concentrated by turbulence for each chondrite, finding excellent matches to each chondrites's mean chondrule diameter. These consistencies imply meteorite parent bodies assembled quickly from local materials concentrated by turbulence, and usually did not migrate far. We predict CI chondrites are depleted in refractory lithophile elements relative to the Sun, by about 12% (0.06 dex). We constrain the variation of turbulence parameter α in the disk, and find a limited role for magnetorotational instability, favoring hydrodynamical instabilities in the outer disk, plus magnetic disk winds in the inner disk. Between 3 and 4 Myr at least, gas persisted outside Jupiter but was depleted inside it, and the solar nebula was a transition disk.

Accretion of differentiated achondritic and aqueously altered chondritic materials in the early solar system—Significance of an igneous fragment in the CM chondrite NWA 12651

“…This is supported by the models of Desch et al. (), which suggest that the outward movement of Jupiter began shortly before the CB chondrites were produced by a catastrophic impact. If the igneous fragment was formed within the or close to the formation region of CB chondrites, it was also formed beyond Jupiter in the carbonaceous chondrite region.…”

“…Based on Mo-isotopes, Budde et al (2016) showed that CB chondrites belong to the group of carbonaceous chondrites and were most likely formed beyond Jupiter together with CM, CO, CK, CV, CB, and CR chondrites. This is supported by the models of Desch et al (2018), which suggest that the outward movement of Jupiter began shortly before the CB chondrites were produced by a catastrophic impact. If the igneous fragment was formed within the or close to the formation region of CB chondrites, it was also formed beyond Jupiter in the carbonaceous chondrite region.…”

“…; Desch et al. ) and differentiated bodies existed very early in the solar system and accreted before the chondritic bodies, for example, ureilites: accretion time 0.6–1.6 Ma (Budde et al. ; Wilson and Goodrich ), angrites: accretion time <1–2 Ma after CAIs (Baker et al.…”

Fingerprints of the Protosolar Cloud Collapse in the Solar System. II. Nucleosynthetic Anomalies in Meteorites

“…A popular add-on in recent literature is to consider that the aforementioned Jupiter-carved gap pressure maximum filtered out dust drifting inward past it (e.g. Desch et al 2018;Nanne et al 2019), sealing off the inner disk from the outer disk. It is uncertain, though, whether the dust flow would be significantly interrupted given the size sensitivity of this concentration process (Haugbølle et al 2019).…”

“…Since the space-time ordering of the different chondrite groups, or even the above broad superclans, is anything but understood (e.g . Wood 2005;Chambers 2006;Jacquet 2014b;Desch et al 2018), these isotopic systematics represent critical constraints to rationalize.…”