Contemporary formation of early Solar System planetesimals at two distinct radial locations

Morbidelli, Alessandro; Baillié, K.; Batygin, Konstantin; Charnoz, Sébastien; Guillot, T.; Rubie, D. C.; Kleine, T.

doi:10.1038/s41550-021-01517-7

Cited by 90 publications

(67 citation statements)

References 69 publications

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“…This is plausible within models where Jupiter would form from a ring of planetesimals around the water-ice line that extends up to 10-15 au (e.g. Izidoro et al 2021b, see also Drażkowska & Dullemond (2018); Morbidelli et al (2022)). Alternatively, Jupiter could have migrated from beyond 15 au only if very few planetesimals would have formed between the water-ice line and its original orbit (sub-MMSN cases represented by black dots in Figure 3; M disk 2.44 M ⊕ for 0.5 MMSN, fpl = 0.1, a init Jup = 20 au, a disk = 5-18 au; and M disk 3.38 M ⊕ when 0.5 MMSN, fpl = 0.1, a init Jup = 25 au, a disk = 5-23 au; Figure 1B).…”

Section: Modelmentioning

confidence: 86%

“…This separation of the NC and CC groups is often called the NC-CC isotopic dichotomy. Recent results further indicate that CC parent bodies (due to their highly oxidized iron core) formed in a wet environment, i.e., beyond or at the water-ice line, whereas NC parent bodies (with nonoxidized iron cores) formed in a dry environment, i.e., interior to the water-ice line (Bermingham et al 2020;Morbidelli et al 2022). It has also been measured that the amount of CC material delivered for both Earth and Mars was on the order of a few percent in mass (e.g.…”

Section: Implications From Generated Dust and Pebble-sized Fragmentsmentioning

confidence: 98%

“…We consider our planetesimals to be made of ice (Benz & Asphaug 1999). This is because we are assuming that they formed beyond the water-ice line, which is predicted to be interior to 5 au (Lambrechts & Johansen 2014;Drażkowska & Alibert 2017) by the time that outer solar system planetesimals formed (≈ 0.5-1 Myr after calcium-aluminium-inclusion -CAI; Lichtenberg et al 2021;Izidoro et al 2021b;Morbidelli et al 2022).…”

Section: Modelmentioning

confidence: 99%

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Implications of Jupiter Inward Gas-driven Migration for the Inner Solar System

Deienno¹,

Izidoro²,

Morbidelli³

et al. 2022

ApJL

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The migration history of Jupiter in the Sun’s natal disk remains poorly constrained. Here we consider how Jupiter’s migration affects small-body reservoirs and how this constrains its original orbital distance from the Sun. We study the implications of large-scale and inward radial migration of Jupiter for the inner solar system while considering the effects of collisional evolution of planetesimals. We use analytical prescriptions to simulate the growth and migration of Jupiter in the gas disk. We assume the existence of a planetesimal disk inside Jupiter’s initial orbit. This planetesimal disk received an initial total mass and size–frequency distribution (SFD). Planetesimals feel the effects of aerodynamic gas drag and collide with one another, mostly while shepherded by the migrating Jupiter. Our main goal is to measure the amount of mass in planetesimals implanted into the main asteroid belt (MAB) and the SFD of the implanted population. We also monitor the amount of dust produced during planetesimal collisions. We find that the SFD of the planetesimal population implanted into the MAB tends to resemble that of the original planetesimal population interior to Jupiter. We also find that unless very little or no mass existed between 5 au and Jupiter’s original orbit, it would be difficult to reconcile the current low mass of the MAB with the possibility that Jupiter migrated from distances beyond 15 au. This is because the fraction of the original disk mass that gets implanted into the MAB is very large. Finally, we discuss the implications of our results in terms of dust production to the so-called NC–CC isotopic dichotomy.

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Section: Modelmentioning

confidence: 86%

Section: Implications From Generated Dust and Pebble-sized Fragmentsmentioning

confidence: 98%

Section: Modelmentioning

confidence: 99%

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Implications of Jupiter Inward Gas-driven Migration for the Inner Solar System

Deienno¹,

Izidoro²,

Morbidelli³

et al. 2022

ApJL

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“…Despite the stark difference in characteristic Stokes number that ensues across the water-ice sublimation front, however, planetesimal formation is expected to operate efficiently in the inner and outer regions of the disk alike. In particular, assuming parameters similar to those derived herein (i.e., s • ∼ mm in the inner disk, s • ∼ cm in the inner disk,) recent work of Morbidelli et al (2021) has demonstrated how radial con-centration of solids near the silicate and H 2 O sublimation lines naturally leads to the contemporaneous generation of rocky and icy planetesimals through gravito-hydrodynamic instabilities (see also Drążkowska et al 2016;Izidoro et al 2021).…”

Section: Discussionmentioning

confidence: 64%

A Self-Consistent Model for Dust-Gas Coupling in Protoplanetary Disks

Batygin¹,

Morbidelli²

2022

Preprint

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Various physical processes that ensue within protoplanetary disks -including vertical settling of icy/rocky grains, radial drift of solids, planetesimal formation, as well as planetary accretion itself -are facilitated by hydrodynamic interactions between H/He gas and high-Z dust. The Stokes number, which quantifies the strength of dust-gas coupling, thus plays a central role in protoplanetary disk evolution, and its poor determination constitutes an important source of uncertainty within the theory of planet formation. In this work, we present a simple model for dust-gas coupling, and demonstrate that for a specified combination of the nebular accretion rate, Ṁ , and turbulence parameter, α, the radial profile of the Stokes number can be calculated uniquely. Our model indicates that the Stokes number grows sub-linearly with orbital radius, but increases dramatically across the water-ice line. For fiducial protoplanetary disk parameters of Ṁ = 10 −8 M /year and α = 10 −3 , our theory yields characteristic values of the Stokes number on the order of St ∼ 10 −4 (corresponding to ∼mm-sized silicate dust) in the inner nebula and St ∼ 10 −1 (corresponding to ∼few-cm-sized icy grains), in the outer regions of the disk. Accordingly, solids are expected to settle into a thin sub-disk at large stellocentric distances, while remaining vertically well-mixed inside the ice line.

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“…The distribution of initial temperatures, and hence compositions of accreted planetesimals and embryos, controlled the composition of the Earth. In order to achieve sufficient temperatures in these precursor bodies, either by heating in the disk and/or 26 Al decay, they must have formed by ~1 Myr, a timescale that is consistent with radiometric ages for volatile depletion 39,41 and protoplanetary disk models 37,38 . Whether precursor body compositions were set by nebular condensation or planetesimal evaporation could be discriminated by holistic models of the growth of planets from the dust-to embryo stages.…”

Section: Figure 2 | Timing Of Element Accretion To the Earth As A Fun...mentioning

confidence: 90%

Stochastic accretion of the Earth

et al. 2022

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Earth is depleted in volatile elements relative to chondritic meteorites, its possible building blocks. The extent of this depletion increases with decreasing condensation temperature, and is approximated by a cumulative normal distribution, unlike that in any chondrite. However, moderately volatile elements, occupying the mid-range of the distribution, have chondritic isotope ratios, contrary to that expected from loss by partial vaporisation/condensation. Here we reconcile these observations by showing, using N-body simulations, that Earth accreted stochastically from many precursor bodies whose variable compositions reflect the temperatures at which they formed. Impact-induced atmospheric loss was efficient only when the proto-Earth was small, and elements that accreted thereafter retain near-chondritic isotope ratios. Earth's composition is reproduced when initial temperatures of planetesimal-to embryo-sized bodies are set by disk accretion rates of (1.08±0.17)×10 -7 solar masses/yr, although they may be perturbed by 26 Al heating on bodies formed at different times. The model implies a heliocentric gradient in composition and rapid planetesimal formation within ~1 Myr, in accord with radiometric volatile depletion ages of Earth.

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Contemporary formation of early Solar System planetesimals at two distinct radial locations

Cited by 90 publications

References 69 publications

Implications of Jupiter Inward Gas-driven Migration for the Inner Solar System

Implications of Jupiter Inward Gas-driven Migration for the Inner Solar System

A Self-Consistent Model for Dust-Gas Coupling in Protoplanetary Disks

Stochastic accretion of the Earth

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