Formation of the Galilean Satellites: Conditions of Accretion

Canup, R. M.; Ward, William R.

doi:10.1086/344684

Cited by 397 publications

(643 citation statements)

References 64 publications

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“…In the case of a planet at Jupiter's orbit, the change of the orbital direction takes place before planetesimals spiral into the planet when ζ 10 −5 . The above range of ζ corresponds to r s 10 m if we assume the gas density based on the gas-starved disk model (Canup & Ward 2002). Figure 9 shows the surface number density of planetesimals captured into retrograde orbit as a function of radial distance for the cases with ζ = 10 −4 and 10 −5 .…”

Section: Radial Distribution Of Captured Planetesimalsmentioning

confidence: 99%

Distribution of Captured Planetesimals in Circumplanetary Gas Disks and Implications for Accretion of Regular Satellites

Suetsugu

Ohtsuki

2017

ApJ

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Regular satellites of giant planets are formed by accretion of solid bodies in circumplanetary disks. Planetesimals that are moving on heliocentric orbits and are sufficiently large to be decoupled from the flow of the protoplanetary gas disk can be captured by gas drag from the circumplanetary disk. In the present work, we examine the distribution of captured planetesimals in circumplanetary disks using orbital integrations. We find that the number of captured planetesimals reaches an equilibrium state as a balance between continuous capture and orbital decay into the planet. The number of planetesimals captured into retrograde orbits is much smaller than those on prograde orbits, because the former ones experience strong headwind and spiral into the planet rapidly. We find that the surface number density of planetesimals at the current radial location of regular satellites can be significantly enhanced by gas drag capture, depending on the velocity dispersions of planetesimals and the width of the gap in the protoplanetary disk. Using a simple model, we also examine the ratio of the surface densities of dust and captured planetesimals in the circumplanetary disk, and find that solid material at the current location of regular satellites can be dominated by captured planetesimals when the velocity dispersion of planetesimals is rather small and a wide gap is not formed in the protoplanetary disk. In this case, captured planetesimals in such a region can grow by mutual collision before spiraling into the planet, and would contribute to the growth of regular satellites.

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Section: Radial Distribution Of Captured Planetesimalsmentioning

confidence: 99%

Distribution of Captured Planetesimals in Circumplanetary Gas Disks and Implications for Accretion of Regular Satellites

Suetsugu

Ohtsuki

2017

ApJ

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“…Initially, giant planets were thought to have formed within a subnebula that was significantly warmer than the PSN and dense enough to convert CO and N 2 from the PSN to CH 4 and NH 3 (Prinn and Fegley 1989). However, Canup and Ward (2002) found that the subnebula of Jupiter must have had a gas density that was orders of magnitudes lower than previously thought. Therefore, the subnebula was probably not dense enough to efficiently convert CO to CH 4 and N 2 to NH 3 (Mousis et al 2002;Alibert and Mousis 2007).…”

Section: Titan Enceladus and Giant Planet Satellitesmentioning

confidence: 57%

“…As discussed earlier, the regular Jovian satellites are presumed to have formed in a circumplanetary nebula that was accreting material from the PSN (Canup and Ward 2002).…”

Section: The Galilean Satellitesmentioning

confidence: 96%

“…Lunine and Stevenson 1982), and that the ice-to-rock ratios of Jupiter's satellites indicate their formation distance within the subnebula (e.g. Canup and Ward 2002;Mousis and Gautier 2004). However, the discovery that Amalthea, a small regular moon orbiting closer to Jupiter than Io, had a higher ice-to-rock ratio than the Galilean satellites (Anderson et al 2005) challenged this assumption.…”

Section: The Galilean Satellitesmentioning

confidence: 99%

“…This parameter is either an indication of their formation distance in Jupiter's subnebula (e.g. Canup and Ward 2002;Mousis and Gautier 2004) or they initially had high ice-to-rock ratios, and have lost part or all of their ice inventory as a result of tidal heating (Estrada et al 2009). Due to extensive thermal processing and radiolitic chemistry on the surface, it is difficult to provide any further constraints on the origin of these moons based on what is currently known about their composition.…”

Section: Current State Of Knowledge and Limitationsmentioning

confidence: 99%

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Constraints from Comets on the Formation and Volatile Acquisition of the Planets and Satellites

et al. 2015

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Comets play a dual role in understanding the formation and evolution of the solar system. First, the composition of comets provides information about the origin of the giant planets and their moons because comets formed early and their composition is not expected to have evolved significantly since formation. They, therefore serve as a record of conditions during the early stages of solar system formation. Once comets had formed, their orbits were perturbed allowing them to travel into the inner solar system and impact the planets. In this way they contributed to the volatile inventory of planetary atmospheres. We review here how knowledge of comet composition up to the time of the Rosetta mission has contributed to understanding the formation processes of the giant planets, their moons and small icy bodies in the solar system. We also discuss how comets contributed to the volatile inventories of the giant and terrestrial planets.

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White Dwarf Circumstellar Disks: Observations

Farihi¹

2011

White Dwarf Atmospheres and Circumstellar Environments

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Formation of the Galilean Satellites: Conditions of Accretion

Cited by 397 publications

References 64 publications

Distribution of Captured Planetesimals in Circumplanetary Gas Disks and Implications for Accretion of Regular Satellites

Distribution of Captured Planetesimals in Circumplanetary Gas Disks and Implications for Accretion of Regular Satellites

Constraints from Comets on the Formation and Volatile Acquisition of the Planets and Satellites

White Dwarf Circumstellar Disks: Observations

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