Gas Dissipation from the Protosatellite Disk of Jupiter

Makalkin, A. B.; Ruskol, E. L.

doi:10.1023/b:sols.0000007948.88258.45

Cited by 11 publications

(17 citation statements)

References 17 publications

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“…Canup and Ward (2002) showed that low-mass models should be preferred. The same conclusion was made by Makalkin and Ruskol (2003) from analyzing the time of gas dissipation from a protoplanetary disk. For massive disk models, the time of the gas dissipation is longer than the time of existence of the Solar System.…”

Section: The Fe/si Ratio In Galilean Satellitessupporting

confidence: 65%

“…The growth of the ç 2 é content with increasing distance from a central body is confirmed by a model of heating the interior of a satellite swarm by a hot giant planet (Ruskol, 1982(Ruskol, , 2003Pollack and Fanale, 1986) and explains why the densities of the inner and outer satellites differ so much. This is because the concentration of petrogenic elements condensing during the disk cooling must either be nearly constant or decrease, while concentrations of volatiles and ices must increase with increasing orbital distance.…”

Section: The Fe/si Ratio In Galilean Satellitesmentioning

confidence: 73%

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Models of the Internal Structure of Callisto

Kuskov

Kronrod

2005

Sol Syst Res

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Models of the internal structure of Callisto were constructed and the extent of its differentiation was determined based on geophysical information from the Galileo spacecraft (the mass, the radius, the mean density, and the moment of inertia), geochemical data (the chemical composition of meteorites), and the equations of state of water, ices, and meteoritic material. The thickness and the phase state of the water-ice shell were defined as well as the ice concentrations in the rock-ice mantle and the bulk concentration of H 2 O. The constraints on the density distribution in the mantle and the size of the rock-iron core were derived. We considered models of the internal structure of Callisto in which the presence of a continuous ice shell was assumed (models without ocean) and models with an internal ocean. We demonstrated that it is possible to apply three-layer models with an icy shell up to 320 km in thickness and a rock-iron core in different combinations with a rock-ice mantle. These models do not reject a two-layer structure of Callisto (an ice lithosphere plus a rock-ice mantle or a rock-ice mantle plus a rock-iron core) and a one-layer model of the satellite composed only of a rock-ice mantle with an ice concentration that is variable in depth. Taking into account the chemically bound water, the bulk content of H 2 O in the satellite is found to be 49-55 wt %. For the model with an internal ocean, the geophysically allowed thickness of the water-ice shell of Callisto was estimated to be 270-315 km with thicknesses of the icy crust and the underlying water layer of 135-150 and 120-180 km, respectively. The results of reconstruction of the composition and structure of the regular satellites of Jupiter allow us to conclude that they were possibly formed from material whose composition was close to ordinary L/LL chondrites at relatively low temperatures, lower than the temperature of evaporation of iron and Fe-Mg silicates.

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Section: The Fe/si Ratio In Galilean Satellitessupporting

confidence: 65%

Section: The Fe/si Ratio In Galilean Satellitesmentioning

confidence: 73%

Models of the Internal Structure of Callisto

Kuskov

Kronrod

2005

Sol Syst Res

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“…We here focus on the "gas-starved" model of an actively supplied circumplanetary disk (CPD; Makalkin et al 1999;Canup & Ward 2002) and determine the time-dependent radial position of the H 2 O ice line. There are several reasons why water ice lines could play a fundamental role in the formation of giant moons.…”

Section: Contextmentioning

confidence: 99%

Alpha-spectrometry and fractal analysis of surface micro-images for characterisation of porous materials used in manufacture of targets for laser plasma experiments

Аушев¹,

Баринов²,

Vasin³

et al. 2015

Quantum Electron.

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Most of the exoplanets with known masses at Earth-like distances to Sun-like stars are heavier than Jupiter, which raises the question of whether such planets are accompanied by detectable, possibly habitable moons. Here we simulate the accretion disks around super-Jovian planets and find that giant moons with masses similar to Mars can form. Our results suggest that the Galilean moons formed during the final stages of accretion onto Jupiter, when the circumjovian disk was sufficiently cool. In contrast to other studies, with our assumptions, we show that Jupiter was still feeding from the circumsolar disk and that its principal moons cannot have formed after the complete photoevaporation of the circumsolar nebula. To counteract the steady loss of moons into the planet due to type I migration, we propose that the water ice line around Jupiter and super-Jovian exoplanets acted as a migration trap for moons. Heat transitions, however, cross the disk during the gap opening within ≈10 4 years, which makes them inefficient as moon traps and indicates a fundamental difference between planet and moon formation. We find that icy moons larger than the smallest known exoplanet can form at about 15-30 Jupiter radii around super-Jovian planets. Their size implies detectability by the Kepler and PLATO space telescopes as well as by the European Extremely Large Telescope. Observations of such giant exomoons would be a novel gateway to understanding planet formation, as moons carry information about the accretion history of their planets.

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“…An analysis of the viscous evolution and dispersal of the disk, similar to that accomplished in this section for the protoplanetary disk, was earlier performed for the protosatellite disk of Jupiter (Makalkin and Ruskol, 2003), the parameters of which were obtained using the current models of the interior structure of the Galilean satellites (Kuskov and Kronrod, 2001).…”

Section: Viscous Evolution and Dispersalmentioning

confidence: 99%

The specific features of the evolution of the viscous protoplanetary circumsolar disk

Makalkin

2004

Sol Syst Res

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The problem of angular-momentum and mass transport in the disk is discussed and the disk viscosity is estimated. The evolution of the gas-dust protoplanetary disk at the stage of its formation inside the protostellar (protosolar) accretion envelope is considered. The conditions for the radial growth of the disk are estimated. For the subsequent period, when the central star (young Sun) is in the T Tauri phase, the temporal variations of the radius, mass, and the surface density of the disk, as well as the total mass flux from the disk onto the star (Sun), i.e., the mass accretion rate, are evaluated. The constraints on the initial value of the angular momentum of the protoplanetary circumsolar disk (that is, on the angular momentum of the protosolar cloud) are discussed with due regard for cosmochemical data.

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Gas Dissipation from the Protosatellite Disk of Jupiter

Cited by 11 publications

References 17 publications

Models of the Internal Structure of Callisto

Models of the Internal Structure of Callisto

Alpha-spectrometry and fractal analysis of surface micro-images for characterisation of porous materials used in manufacture of targets for laser plasma experiments

The specific features of the evolution of the viscous protoplanetary circumsolar disk

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