The dynamics of Jupiter and Saturn in the gaseous protoplanetary disk

Morbidelli, Alessandro; Crida, A.

doi:10.1016/j.icarus.2007.04.001

Cited by 228 publications

(129 citation statements)

References 36 publications

(42 reference statements)

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“…Once in 2/3 resonance configuration, the planets cease migrating inwards. It was shown in Morbidelli and Crida (2007) that the subsequent orbital evolution depends on the properties of the disk, particularly the scale height. In general, both planets migrate outwards together, on a short timescale.…”

Section: The Dynamics Of the Giant Planets In A Gas-diskmentioning

confidence: 99%

“…However, if the disk is very thick, the migration rate is very slow, as in Fig 3. For some appropriate disk thickness there is essentially no migration. 2 The presence of asteroids inside of Jupiter's orbit suggests at first sight that Jupiter never 2 Notice that, for two giant planets to avoid inward migration by this mechanism, it is essential that the mass of the outer planet is a fraction of the mass of the inner planet, as in the Jupiter-Saturn case (Masset and Snellgrove, 2001;Morbidelli and Crida, 2007). Planets of comparable masses or with a reversed mass ratio do migrate towards the central star also after resonance trapping.…”

Section: The Dynamics Of the Giant Planets In A Gas-diskmentioning

confidence: 99%

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A coherent and comprehensive model of the evolution of the outer Solar System

Morbidelli¹

2010

Comptes Rendus. Physique

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Since the discovery of the first extra-solar planets, we are confronted with the puzzling diversity of planetary systems. Processes like planet radial migration in gasdisks and planetary orbital instabilities, often invoked to explain the exotic orbits of the extra-solar planets, at first sight do not seem to have played a role in our system.In reality, though, there are several aspects in the structure of our Solar System that cannot be explained in the classic scenario of in-situ formation and smooth evolution of the giant planets. This paper describes a new view of the evolution of the outer Solar System that emerges from the so-called 'Nice model' and its recent extensions. The story provided by this model describes a very "dynamical" Solar System, with giant planets affected by both radial migrations and a temporary orbital instability. Thus, the diversity between our system and those found so far around other stars does not seem to be due to different processes that operated here and elsewhere, but rather stems from the strong sensitivity of chaotic evolutions to small differences in the initial and environmental conditions.In press in "C.R. Physique de l'Académie des Sciences".

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Section: The Dynamics Of the Giant Planets In A Gas-diskmentioning

confidence: 99%

Section: The Dynamics Of the Giant Planets In A Gas-diskmentioning

confidence: 99%

A coherent and comprehensive model of the evolution of the outer Solar System

Morbidelli¹

2010

Comptes Rendus. Physique

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“…It should be noted that for models with H DZ 0, and provided that the viscosity is high enough in the live-zone, a migration rate which is lower than the inward drift velocity in the active region can make the disk material from this region flow across the gap. This not only enables the inner disk to be continuously supplied with gas but also creates a positive corotation torque on the planet as the gas flows through the gap (Masset & Snellgrove 2001;Morbidelli & Crida 2007).…”

Section: Orbital Evolution Of Jupiter-mass Planetsmentioning

confidence: 99%

On the growth and orbital evolution of giant planets in layered protoplanetary disks

Nelson

2010

A&A

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Aims. We present the results of hydrodynamic simulations of the growth and orbital evolution of giant planets embedded in a protoplanetary disk with a dead-zone. The aim is to examine to what extent the presence of a dead-zone affects the rates of mass accretion and migration for giant planets. Methods. We performed 3D numerical simulations using a grid-based hydrodynamics code. In these simulations of laminar, nonmagnetised disks, the dead-zone is treated as a region where the vertical profile of the viscosity depends on the distance from the equatorial plane. We consider dead-zones with vertical sizes, H DZ , ranging from 0 to H DZ = 2.3 H, where H is the disk scale-height. For all models, the vertically integrated viscous stress, and the related mass flux through the disk, have the same value (equivalent to 10 −8 M yr −1 ), such that the simulations test the dependence of planetary mass accretion and migration on the vertical distribution of the viscous stress (and mass flux). For each model, an embedded 30 M ⊕ planet on a fixed circular orbit is allowed to accrete gas from the disk. Once the planet mass becomes equal to that of Saturn or Jupiter, we allow the planet orbit to evolve due to gravitational interaction with the disk. Results. We find that the time scale over which a protoplanet grows to become a giant planet is essentially independent of the deadzone size, and depends only on the total rate at which the disk viscously supplies material to the planet. For Saturn-mass planets, the migration rate depends only weakly on the size of the dead-zone for H DZ ≤ 1.5 H, but becomes noticeably slower when H DZ = 2.3 H. This effect is apparently due to the desaturation of corotation torques which originate from residual material in the partial-gap region. For Jupiter-mass planets, there is a clear tendency for the migration to proceed more slowly as the size of the dead-zone increases, with migration rates differing by approximately 40% for models with H DZ = 0 and H DZ = 2.3 H. Conclusions. Our results indicate that for disks models in which the mass accretion rate has a well defined value, the accretion and migration rates for Saturn-and Jovian-mass planets are relatively insensitive to the presence and size of a dead-zone.

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“…However, the assumption that the giant planets orbits had their current semimajor axes when the gas was still present is no longer supported. When embedded in a gas disk, planets migrate relative to each other until a resonance configuration is achieved (Peale & Lee 2002;Kley et al 2009;Ferraz-Mello et al 2003;Masset & Snellgrove 2001;Morbidelli & Crida 2007;Pierens & Nelson 2008). Thus it is believed that the giant planets were in resonance with each other when the gas disk disappeared (Morbidelli et al 2007;Thommes et al 2008a;Batygin & Brown 2010) which causes problems in understanding the consequences of the Thommes et al (2008b) model.…”

Section: Introductionmentioning

confidence: 99%

“…When embedded in a gas disk, planets migrate relative to each other until a resonance configuration is achieved (Peale & Lee 2002;Kley et al 2009;Ferraz-Mello et al 2003;Masset & Snellgrove 2001;Morbidelli & Crida 2007;Pierens & Nelson 2008). Thus it is believed that the giant planets were in resonance with each other when the gas disk disappeared (Morbidelli et al 2007;Thommes et al 2008a;Batygin & Brown 2010) which causes problems in understanding the consequences of the Thommes et al (2008b) model. Moreover, the Nagasawa et al (2005) and Thommes et al (2008a) simulations produce the terrestrial planets too quickly (∼10 Myr), compared to the timing of moon formation indicated by the 182 Hf-182 W chronometer (>30 Myr and most likely >50 Myr; Kleine et al 2009) and they completely deplete the asteroid belt by the combination of resonance sweeping and gas-drag (see also Morishima et al 2010, for a discussion).…”

Section: Introductionmentioning

confidence: 99%

The effect of an early planetesimal-driven migration of the giant planets on terrestrial planet formation

Walsh

Morbidelli

2011

A&A

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The migration of the giant planets due to the scattering of planetesimals causes powerful resonances to move through the asteroid belt and the terrestrial planet region. Exactly when and how the giant planets migrated is not well known. In this paper we present results of an investigation of the formation of the terrestrial planets during and after the migration of the giant planets. The latter is assumed to have occurred immediately after the dissipation of the nebular disk -i.e. "early" with respect to the timing of the late heavy bombardment (LHB). The presumed cause of our modeled early migration of the giant planets is angular mometum transfer between the planets and scattered planetesimals. Our model forms the terrestrial planets from a disk of material which stretchs from 0.3-4.0 AU, evenly split in mass between planetesimals and planetary embryos. Jupiter and Saturn are initially at 5.4 and 8.7 AU respectively, on orbits with eccentricities comparable to the current ones, and migrate to 5.2 and 9.4 AU with an e-folding time of 5 Myr. Unfortunately, the terrestrial planets formed in the simulations are not good analogs for the current solar system, with Mars typically being much too massive. Moreover, the final distribution of the planetesimals remaining in the asteroid belt is inconsistent with the observed distribution of asteroids. This argues that, even if giant planet migration had occurred early, the real evolution of the giant planets would have to have been of the "jumping-Jupiter" type, i.e. the increase in orbital separation between Jupiter and Saturn had to be dominated by encounters between Jupiter and a third, Neptune-mass planet. This result was already demonstrated for late migrations occuring at the LHB time by previous work, and this paper shows those conclusions hold for early migration as well.

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The dynamics of Jupiter and Saturn in the gaseous protoplanetary disk

Cited by 228 publications

References 36 publications

A coherent and comprehensive model of the evolution of the outer Solar System

A coherent and comprehensive model of the evolution of the outer Solar System

On the growth and orbital evolution of giant planets in layered protoplanetary disks

The effect of an early planetesimal-driven migration of the giant planets on terrestrial planet formation

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