Saturn’s Formation and Early Evolution at the Origin of Jupiter’s Massive Moons

Ronnet, Thomas; Mousis, O.; Vernazza, Pierre; Lunine, Jonathan I.; Crida, A.

doi:10.3847/1538-3881/aabcc7

Cited by 41 publications

(48 citation statements)

References 80 publications

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“…Another important issue is that it is unlikely that the material accreted by a giant planet in the late stages of its formation has a solar dust-to-gas mass ratio, as advocated in the gas-starved models (see Ronnet et al 2018, for a discussion). Above a mass of typically a few ∼10 M ⊕ , a protoplanet starts to significantly perturb the gas disk in its vicinity, opening a shallow gap whose outer edge acts as a barrier for drifting dust grains (Morbidelli & Nesvorny 2012;.…”

Section: Motivationmentioning

confidence: 99%

Formation of moon systems around giant planets

Ronnet

Johansen

2020

A&A

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The four major satellites of Jupiter, known as the Galilean moons, and Saturn’s most massive satellite, Titan, are believed to have formed in a predominantly gaseous circum-planetary disk during the last stages of formation of their parent planet. Pebbles from the protoplanetary disk are blocked from flowing into the circumplanetary disk by the positive pressure gradient at the outer edge of the planetary gap, so the gas drag assisted capture of planetesimals should be the main contributor to the delivery of solids onto circum-planetary disks. However, a consistent framework for the subsequent accretion of the moons remains to be built. Here, we use numerical integrations to show that most planetesimals that are captured within a circum-planetary disk are strongly ablated due to the frictional heating they experience, thus supplying the disk with small dust grains, whereas only a small fraction “survives” their capture. We then constructed a simple model of a circum-planetary disk supplied by ablation, where the flux of solids through the disk is at equilibrium with the ablation supply rate, and we investigate the formation of moons in such disks. We show that the growth of satellites is mainly driven by accretion of the pebbles that coagulate from the ablated material. The pebble-accreting protosatellites rapidly migrate inward and pile up in resonant chains at the inner edge of the circum-planetary disk. We propose that dynamical instabilities in these resonant chains are at the origin of the different architectures of Jupiter’s and Saturn’s moon systems. The assembly of moon systems through pebble accretion can therefore be seen as a down-scaled manifestation of the same process that forms systems of super-Earths and terrestrial-mass planets around solar-type stars and M-dwarfs.

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Section: Motivationmentioning

confidence: 99%

Formation of moon systems around giant planets

Ronnet

Johansen

2020

A&A

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“…In such a situation, concentration of grains in pressure bumps can promote the growth of already-existing planetesimals/protoplanets via pebble accretion (Johansen & Lacerda 2010;Ormel & Klahr 2010). In fact, more than 20 Earth-masses of solid particles are collected in the outermost pressure bump in Model 1, potentially facilitating the formation of a second-generation (giant) planet there (Lyra et al 2009;Ronnet et al 2018; see Figure 6. Simulated millimeter continuum observations of the three models with (first row) 0".025, (second row) 0".13, (third row) 0".24, and (fourth row) 0".40 angular resolution.…”

Section: Disk Morphology In Millimeter Continuummentioning

confidence: 99%

Diverse Protoplanetary Disk Morphology Produced by a Jupiter-mass Planet

Bae

Pinilla

Birnstiel

2018

ApJL

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Combining hydrodynamic planet-disk interaction simulations with dust evolution models, we show that protoplanetary disks having a giant planet can reveal diverse morphology in (sub-)millimeter continuum, including a full disk without significant radial structure, a transition disk with an inner cavity, a disk with a single gap and a central continuum peak, and a disk with multiple rings and gaps. Such a diversity originates from (1) the level of viscous transport in the disk which determines the number of gaps a planet can open; (2) the size and spatial distributions of grains determined by the coagulation, fragmentation, and radial drift, which in turn affects the emmisivity of the disk at (sub-)millimeter wavelengths; and (3) the angular resolution used to observe the disk. In particular, our results show that disks having the same underlying gas distribution can have very different grain size/spatial distributions and thus appearance in continuum, depending on the interplay among coagulation, fragmentation, and radial drift. This suggests that proper treatments for the grain growth have to be included in models of protoplanetary disks concerning continuum properties and that complementary molecular line observations are highly desired in addition to continuum observations to reveal the true nature of disks. The fact that a single planet can produce diverse disk morphology emphasizes the need to search for more direct, localized signatures of planets in order to confirm (or dispute) the planetary origin of observed ringed substructures.

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“…We aim to find a way to form a system with only one large moon in a CPD. The feasibility of satellitesimal formation has been examined by Shibaike et al (2017) and delivery of solid matereal to a CPD has been discussed by Fujita et al (2012); Tanigawa et al (2014); Suetsugu & Ohtsuki (2017); Ronnet et al (2018). We focus on the later stage of the satellite formation and investigate the orbital evolution of the moons in a dissipating CPD to determine the final appearance of the system.…”

Section: Introductionmentioning

confidence: 99%

Formation of single-moon systems around gas giants

Fujii

Ogihara

2020

A&A

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Context. Several mechanisms have been proposed to explain the formation process of satellite systems, and relatively large moons are thought to be born in circumplanetary disks. Making a single-moon system is known to be more difficult than multiple-moon or moonless systems. Aims. We aim to find a way to form a system with a single large moon, such as Titan around Saturn. We examine the orbital migration of moons, which change their direction and speed depending on the properties of circumplanetary disks. Methods. We modeled dissipating circumplanetary disks with taking the effect of temperature structures into account and calculated the orbital evolution of Titan-mass satellites in the final evolution stage of various circumplanetary disks. We also performed N-body simulations of systems that initially had multiple satellites to see whether single-moon systems remained at the end. Results. The radial slope of the disk-temperature structure characterized by the dust opacity produces a patch of orbits in which the Titan-mass moons cease inward migration and even migrate outward in a certain range of the disk viscosity. The patch assists moons initially located in the outer orbits to remain in the disk, while those in the inner orbits fall onto the planet. Conclusions. We demonstrate for the first time that systems can form that have only one large moon around giant planet. Our N-body simulations suggest satellite formation was not efficient in the outer radii of circumplanetary disks.

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Saturn’s Formation and Early Evolution at the Origin of Jupiter’s Massive Moons

Cited by 41 publications

References 80 publications

Formation of moon systems around giant planets

Formation of moon systems around giant planets

Diverse Protoplanetary Disk Morphology Produced by a Jupiter-mass Planet

Formation of single-moon systems around gas giants

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