Improved torque formula for low- and intermediate-mass planetary migration

Jimenez, Maria Alejandra; Masset, F.

doi:10.1093/mnras/stx1946

Cited by 98 publications

(168 citation statements)

References 39 publications

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“…In general, C can take on a range of values (e.g., Casoli & Masset 2009;Paardekooper et al 2010Paardekooper et al , 2011Jiménez & Masset 2017), but is generally positive in isothermal disks. Here, we choose C=2 given by the three-dimensional simulations of .…”

Section: Stage I: Core Growth and Type I Migrationmentioning

confidence: 99%

Inner Super-Earths, Outer Gas Giants: How Pebble Isolation and Migration Feedback Keep Jupiters Cold

Fung

Lee

2018

ApJ

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The majority of gas giants (planets of masses 10 2 M ⊕ ) are found to reside at distances beyond ∼1 au from their host stars. Within 1 au, the planetary population is dominated by super-Earths of 2-20M ⊕ . We show that this dichotomy between inner super-Earths and outer gas giants can be naturally explained should they form in nearly inviscid disks. In laminar disks, a planet can more easily repel disk gas away from its orbit. The feedback torque from the pile-up of gas inside the planet's orbit slows down and eventually halts migration. A pressure bump outside the planet's orbit traps pebbles and solids, starving the core. Gas giants are born cold and stay cold: more massive cores are preferentially formed at larger distances, and they barely migrate under disk feedback. We demonstrate this using two-dimensional hydrodynamical simulations of disk-planet interaction lasting up to 10 5 years: we track planet migration and pebble accretion until both come to an end by disk feedback. Whether cores undergo runaway gas accretion to become gas giants or not is determined by computing one-dimensional gas accretion models. Our simulations show that in an inviscid minimum mass solar nebula, gas giants do not form inside ∼0.5au, nor can they migrate there while the disk is present. We also explore the dependence on disk mass and find that gas giants form further out in less massive disks.

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Section: Stage I: Core Growth and Type I Migrationmentioning

confidence: 99%

Inner Super-Earths, Outer Gas Giants: How Pebble Isolation and Migration Feedback Keep Jupiters Cold

Fung

Lee

2018

ApJ

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“…For information about the calculation of type II migration timescales in this paper, see Appendix D. A simplification in these simulations is that the planets move in circular orbits with vanishing inclinations. This is a sensible approximation, as eccentricity and inclination are damped quite quickly by the gas disk (Bitsch & Kley 2010 Paardekooper et al (2011) and Jiménez & Masset (2017) both performed hydrodynamical simulations in non-barotropic disks with finite viscosity and constant thermal diffusion to derive their formulae. The major difference is that Paardekooper et al (2011) made two-dimensional simulations, while Jiménez & Masset (2017) updated their findings based on three-dimensional disks.…”

Section: Planetary Growth and Migration Modelsmentioning

confidence: 99%

“…The second contribution is the barotropic torque, resulting from the surface density gradient. All of the above components are incorporated in Jiménez & Masset (2017) as well, although the barotropic torque is called vortensity torque in their formulation. Additionally, there is the temperature torque as another contribution of the midplane temperature gradient.…”

Section: Planetary Growth and Migration Modelsmentioning

confidence: 99%

“…Additionally, there is the temperature torque as another contribution of the midplane temperature gradient. Finally, Jiménez & Masset (2017) introduced the viscous coupling term, a result of viscous production of vortensity at the density jumps at the seperatrices of the horseshoe region. We ought to keep in mind that these formulae describe type I migration.…”

Section: Planetary Growth and Migration Modelsmentioning

confidence: 99%

“…However, planet formation simulations cannot incorporate 2D or 3D hydrodynamical simulations to accurately calculate the torques over millions of years. Thus, the planet formation simulations rely on torque formulae derived from hydrodynamical simulations, such as * e-mail: Thomas.Baumann@cebaumann.de Masset & Casoli (2010), Paardekooper et al (2011), or Jiménez & Masset (2017.…”

Section: Introductionmentioning

confidence: 99%

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Influence of migration models and thermal torque on planetary growth in the pebble accretion scenario

Baumann

Bitsch

2020

A&A

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Low-mass planets that are in the process of growing larger within protoplanetary disks exchange torques with the disk and change their semi-major axis accordingly. This process is called type I migration and is strongly dependent on the underlying disk structure. As a result, there are many uncertainties about planetary migration in general. In a number of simulations, the current type I migration rates lead to planets reaching the inner edge of the disk within the disk lifetime. A new kind of torque exchange between planet and disk, the thermal torque, aims to slow down inward migration via the heating torque. The heating torque may even cause planets to migrate outwards, if the planetary luminosity is large enough. Here, we study the influence on planetary migration of the thermal torque on top of previous type I models. We find that the formula of Paardekooper et al. (2011) allows for more outward migration than that of Jiménez & Masset (2017) in most configurations, but we also find that planets evolve to very similar mass and final orbital radius using both formulae in a single planet-formation scenario, including pebble and gas accretion. Adding the thermal torque can introduce new, but small, regions of outwards migration if the accretion rates onto the planet correspond to typical solid accretion rates following the pebble accretion scenario. If the accretion rates onto the planets become very large, as could be the case in environments with large pebble fluxes (e.g., high-metallicity environments), the thermal torque can allow more efficient outward migration. However, even then, the changes for the final mass and orbital positions in our planet formation scenario are quite small. This implies that for single planet evolution scenarios, the influence of the heating torque is probably negligible.

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Web of resonances and possible path of evolution of the small Uranian satellites

Charalambous

Giuppone

Guilera

2022

Astrophys Space Sci

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Satellite systems around giant planets are immersed in a region of complex resonant configurations. Understanding the role of satellite resonances contributes to comprehending the dynamical processes in planetary formation and posterior evolution. Our main goal is to analyse the resonant structure of small moons around Uranus and propose different scenarios able to describe the current configuration of these satellites. We focus our study on the external members of the regular satellites interior to Miranda, namely Rosalind, Cupid, Belinda, Perdita, Puck, and Mab, respectively. We use N-body integrations to perform dynamical maps to analyse their dynamics and proximity to two-body and three-body mean-motion resonances (MMR). We found a complicated web of low-order resonances amongst them. Employing analytical prescriptions, we analysed the evolution by gas drag and type-I migration in a circumplanetary disc (CPD) to explain different possible histories for these moons. We also model the tidal evolution of these satellites using some crude approximations and found possible paths that could lead to MMRs crossing between pairs of moons. Finally, our simulations show that each mechanism can generate significant satellite radial drift leading to possible resonant capture, depending on the distances and sizes.

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Improved torque formula for low- and intermediate-mass planetary migration

Cited by 98 publications

References 39 publications

Inner Super-Earths, Outer Gas Giants: How Pebble Isolation and Migration Feedback Keep Jupiters Cold

Inner Super-Earths, Outer Gas Giants: How Pebble Isolation and Migration Feedback Keep Jupiters Cold

Influence of migration models and thermal torque on planetary growth in the pebble accretion scenario

Web of resonances and possible path of evolution of the small Uranian satellites

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