Giant Planet Formation and Migration

Paardekooper, Sijme-Jan; Johansen, Anders

doi:10.1007/s11214-018-0472-y

Cited by 25 publications

(13 citation statements)

References 139 publications

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“…This is not a very sharp criterion in practice, and the Type II migration arising in very clean gaps, as typically considered for a Jupiter-like case corresponds to a planet of mass ∼ 10 M 1 . The reader should also note that the various parameters used in the literature for this non-linearity or thermal criterion often differ by small factors of order unity, and some with the same scaling are derived through different physical arguments (Lin & Papaloizou 1993;Korycansky & Papaloizou 1996;Ward 1997;Paardekooper & Johansen 2018) 1 . Feedback and vortices: Where the planet mass is large enough for the wake dissipation to alter the local disc surface density profile, and hence alter the Lindblad torques, the feedback slows planet migration.…”

Section: Migration Behaviour Regimesmentioning

confidence: 99%

Migrating super-Earths in low-viscosity discs: unveiling the roles of feedback, vortices, and laminar accretion flows

McNally

Nelson

Paardekooper

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present the highest resolution study to date of super-Earths migrating in inviscid and low-viscosity discs, motivated by the connection to laminar, wind-driven models of protoplanetary discs. Our models unveil the critical role of vortices in determining the migration behaviour for partial gap-opening planets. Vortices form in pressure maxima at gap edges, and prevent the disc-feedback stopping of migration for intermediate planets in low-viscosity and inviscid discs, contrary to the concept of the 'inertial limit' or 'disc feedback' halting predicted from analytical models. Vortices may also form in the corotation region, and can dramatically modify migration behaviour through direct gravitational interaction with the planet. These features become apparent at high resolution, and for all but the highest viscosities there exist significant difficulties in obtaining numerically converged results. The migration of partial gap-opening planets, however, clearly becomes chaotic for sufficiently low viscosities. At moderate viscosity, a smooth disc-feedback regime is found in which migration can slow substantially, and the migration time-scale observed corresponds to migration being driven by diffusive relaxation of the gap edges. At high viscosity classical Type I migration is recovered. For Jupiter-analogue planets in inviscid discs, a wide, deep gap is formed. Transient Type II migration occurs over radial length-scales corresponding to the gap width, beyond which migration can stall. Finally, we examine the particle trapping driven by structures left in inviscid discs by a migrating planet, and find that particle traps in the form of multiple rings and vortices can persist long after the planet has passed. In this case, the observation of particle traps by submillimetre interferometers such as ALMA cannot be used to infer the current presence of an adjacent planet.

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Section: Migration Behaviour Regimesmentioning

confidence: 99%

Migrating super-Earths in low-viscosity discs: unveiling the roles of feedback, vortices, and laminar accretion flows

McNally

Nelson

Paardekooper

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…Within the broader framework of satellite-disk interactions, a large surface density gradient leads to a dramatic enhancement in the corotation torque. In turn, this effect preferentially pulls the migrating object into the region of higher density(Masset et al 2006;Paardekooper & Johansen 2018). Therefore, the surface density jump envisioned byMosqueira & Estrada (2003a, 2003b) is likely to operate as a reversed planet trap, briefly accelerating-instead of halting-Callisto's orbital decay.5 We note that contrary to this assumption,Sasaki et al (2010) argue that the planetary magnetosphere may effectively truncate the circumplanetary disk, halting the inward migration of satellites at the inner edge.6 The satellite systems of Uranus and Neptune are beyond the scope of our study, as they likely have a distinct origin from the scenario considered herein (see, e.g., the recent work ofIda et al 2020).7 Contrary to accretion disks-where long-term viscous evolution leads to the gradual sinking of nebular material toward the central object-decretion disks are systems where gas and dust are slowly expelled outwards.…”

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confidence: 99%

Formation of Giant Planet Satellites

Batygin

Morbidelli

2020

ApJ

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Recent analyses have shown that the concluding stages of giant planet formation are accompanied by the development of a large-scale meridional flow of gas inside the planetary Hill sphere. This circulation feeds a circumplanetary disk that viscously expels gaseous material back into the parent nebula, maintaining the system in a quasi-steady state. Here, we investigate the formation of natural satellites of Jupiter and Saturn within the framework of this newly outlined picture. We begin by considering the long-term evolution of solid material, and demonstrate that the circumplanetary disk can act as a global dust trap, where s • ∼0.1-10 mm grains achieve a hydrodynamical equilibrium, facilitated by a balance between radial updraft and aerodynamic drag. This process leads to a gradual increase in the system's metallicity, and eventually culminates in the gravitational fragmentation of the outer regions of the solid subdisk into 100 km satellitesimals. Subsequently, satellite conglomeration ensues via pair-wise collisions but is terminated when disk-driven orbital migration removes the growing objects from the satellitesimal feeding zone. The resulting satellite formation cycle can repeat multiple times, until it is brought to an end by photoevaporation of the parent nebula. Numerical simulations of the envisioned formation scenario yield satisfactory agreement between our model and the known properties of the Jovian and Saturnian moons.

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“…The detailed physics of the planet-disk gravitational interaction is a complicated topic (see e.g. the review by Paardekooper & Johansen 2018). Planetary mass is an important parameter that defines the regime of migration.…”

Section: Planet Migration In Gaseous Diskmentioning

confidence: 99%

Planet migration in wind-fed accretion discs in binaries

Kulikova

Попов

Zhuravlev

2019

Monthly Notices of the Royal Astronomical Society

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Planet migration originally refers to protoplanetary disks, which are more massive and dense than typical accretion disks in binary systems. We study planet migration in an accretion disk in a binary system consisting of a solar-like star hosting a planet and a red giant donor star. The accretion disk is fed by a stellar wind. We use the αdisk model and consider that the stellar wind is time-dependent. Assuming the disk is quasi-stationary we calculate its temperature and surface density profiles. In addition to the standard disk model, when matter is captured by the disk at its outer edge, we study the situation when the stellar wind delivers matter on the whole disc surface inside the accretion radius with the rate depending on distance from the central star. Implying that a planet experiences classical type I/II migration we calculate migration time for a planet on a circular orbit coplanar with the disk. Potentially, rapid inward planet migration can result in a planet-star merger which can be accompanied by an optical or/and UV/X-ray transient. We calculate timescale of migration for different parameters of planets and binaries. Our results demonstrate that planets can fall on their host stars within the lifetime of the late-type donor for realistic sets of parameters.

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Giant Planet Formation and Migration

Cited by 25 publications

References 139 publications

Migrating super-Earths in low-viscosity discs: unveiling the roles of feedback, vortices, and laminar accretion flows

Migrating super-Earths in low-viscosity discs: unveiling the roles of feedback, vortices, and laminar accretion flows

Formation of Giant Planet Satellites

Planet migration in wind-fed accretion discs in binaries

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