Formation of the regular satellites of giant planets in an extended gaseous nebula I: subnebula model and accretion of satellites

Mosqueira, I.; Estrada, P. R.

doi:10.1016/s0019-1035(03)00076-9

Cited by 205 publications

(194 citation statements)

References 100 publications

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“…Later studies revised this model and tried to explain the difference between the satellite systems of Jupiter and Saturn (Sasaki et al 2010;Ogihara & Ida 2012). On the other hand, the socalled solid enhanced minimum mass disk model proposed by Mosqueira & Estrada (2003) considers a circumplanetary disk consisting of two different parts of surface density in order to explain the rock-ice ratio of the Galilean satellites. Recently, satellite formation based on this model was examined semi-analytically (Miguel & Ida 2016).…”

Section: Introductionmentioning

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: Introductionmentioning

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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“…Their bulk densities range from a high of 1.6 g/cm^ for Enceladus (Porco et al, 2006) to perhaps as low as 1.0 g/cm^ for Tethys (Dourneau and Baratchart, 1999), betraying compositions of mostly water ice but with formation histories that led to differing non-ice fractions and interior structure. Compositions are likely related to the positions of their formation from Saturn, especially with regard to the fraction of ammonia (e.g., Mosqueira and Estrada, 2003) which is expected to be prevalent in these satellites due to the cool temperatures in the saturnian nebula (Lewis, 1972). The Cassini mission has recently performed close flybys of these moons, confirming that varying degrees of geologic activity (Wagner et al, 2006) were sustained for an extended period of time on these small objects after their formation, and continuing to the present on Enceladus (Porco et al, 2006).…”

Section: Introductionmentioning

confidence: 99%

Arecibo radar observations of Rhea, Dione, Tethys, and Enceladus

Black

Campbell

Carter

2007

Icarus

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“…In view of these studies, particularly Mosqueira & Estrada (2003) and Estrada & Mosqueira (2006), it is therefore quite reasonable to take into account the existence of some si satellites as we did, and to see their evolution during the planetary migration. The second decisive result of Boué & Laskar (2010) is that their satellite must be destabilized after some time, and this is exactly what we have found in this work.…”

Section: The Si Satellitesmentioning

confidence: 85%

“…An additional interesting problem is the current obliquity of Uranus. Mosqueira & Estrada (2003) and Estrada & Mosqueira (2006), in their model of satellite formation, note that regular satellites of Uranus can be formed within a disk of radius ≈57 R U . We note that this value is in quite close agreement with the distances predicted based on our value of a c as we note in Sect.…”

Section: The Si Satellitesmentioning

confidence: 99%

“…These events are related to the satellite formation process (Mosqueira & Estrada 2003;Canup & Ward 2000, planetary migration (including collisions), and dynamical instability. In particular for Uranus, we propose that the results on migrational theory of Tsiganis et al (2005) can provide interesting results in this direction.…”

Section: Regular and Irregular Satellitesmentioning

confidence: 99%

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Effects of the planetary migration on some primordial satellites of the outer planets

Deienno

Yokoyama

Callegari

et al. 2011

A&A

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Context. During the first hundred million years after the formation of our solar system, the four giant planets are believed to have migrated significantly (by up ≈20 AU). The current scenario and dynamics of the satellites of these planets must be the result of both the initial conditions of their formation and this early extensive migrational episode. Aims. We examine the effects of the migration on the primordial satellites of Uranus. Methods. We use the Nice model to generate templates for the evolution of the four giant planets and record the time history of these planets and important close encounters. The satellites are then added to Uranus and these objects are integrated according to the dynamics stored in the templates. Results. We show that Oberon is the outermost regular satellite of Uranus that is able to resist the close encounters during the extensive migrational episode. Some theories predict that Uranus' satellites can form out to a 57 R U distance from the planet, but we show that even those at ≈27 R U from the planet cannot support the instabilities that appeared during migration. Close objects, such as the current regular satellites of Uranus, can survive quite stably and we are able to place some constraints on the masses of the planetesimals that have close encounters. For instance, if an object with mass ≥10 −9 M approaches at distances < ∼ 23 R U from Uranus, the regular satellites can be destabilized or their eccentricities or inclinations excited to some non-compatibles values. We also find that planet-planetesimal close encounters can generate capture. In this way, we present a promising means of explaining the origin of the irregular satellites of Uranus. The importance of the oblateness of the planet, and the Sun for just-captured planetesimals is also shown.

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Formation of the regular satellites of giant planets in an extended gaseous nebula I: subnebula model and accretion of satellites

Cited by 205 publications

References 100 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

Arecibo radar observations of Rhea, Dione, Tethys, and Enceladus

Effects of the planetary migration on some primordial satellites of the outer planets

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