Capture and migration of Jupiter and Saturn in mean motion resonance in a gaseous protoplanetary disc

Chametla, Raúl O.; D’Angelo, Gennaro; Reyes-Ruiz, M.; Sánchez-Salcedo, F. J.

doi:10.1093/mnras/staa260

Cited by 14 publications

(11 citation statements)

References 45 publications

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“…Depending on the shape of the gap created and the migration speed of the low mass planet, the capture in certain resonances might therefore be avoided. The capture in resonance is important for the Grand Tack scenario (Walsh et al 2011), where Jupiter and Saturn get locked in 3:2 or 2:1 resonance and start migrating outward (Masset & Snellgrove 2001;Pierens & Nelson 2008;Raymond et al 2011;Pierens et al 2014;Chametla et al 2020). We discuss in section 5.3 the impact of resonance capture on the structure of our solar system.…”

Section: Migration Mapsmentioning

confidence: 99%

Influence of planetary gas accretion on the shape and depth of gaps in protoplanetary discs

Bergez-Casalou,

Bitsch,

Pierens

et al. 2020

Preprint

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It is well known that giant planets open deep gaps in their natal gaseous protoplanetary discs. However, it is unclear how gas accretion onto growing planets influences the shape and depth of their growing gaps. We perform isothermal hydrodynamical simulations with the Fargo-2D1D code in which planets accrete gas within full discs that range from 0.1 to 260 AU. The gas accretion routine uses a sink cell approach, where we use different accretion rates to cope with the large span of gas accretion rates in the literature. We find that the planetary gas accretion rate increases for larger disc aspect ratios and larger viscosities. Our main result shows that gas accretion has an important impact on the gap opening mass: we find that when the disc responds slowly to a change in planetary mass (i.e. at low viscosity), the gap opening mass scales with the planetary accretion rate, with a higher gas accretion rate resulting in a larger gap opening mass. On the other hand, if the disc response time is short (i.e. at high viscosity), then gas accretion helps the planet carve a deep gap. As a consequence higher planetary gas accretion rates result in smaller gap opening masses. Our results have important implications for the derivation of planet masses from disc observations: depending on the planetary gas accretion rate, the derived masses from ALMA observations might be off by up to a factor 2. We discuss the consequence of the change of the gap opening mass on the evolution of planetary systems by taking the example of the Grand Tack scenario. Planetary gas accretion also impacts the stellar gas accretion, where we find only a small influence due to the presence of a gas accreting planet.

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Section: Migration Mapsmentioning

confidence: 99%

Influence of planetary gas accretion on the shape and depth of gaps in protoplanetary discs

Bergez-Casalou,

Bitsch,

Pierens

et al. 2020

Preprint

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“…Depending on the shape of the gap created and the migration speed of the low-mass planet, the capture in certain resonances might therefore be avoided. The capture in resonance is important for the grand tack scenario (Walsh et al 2011), where Jupiter and Saturn get locked in 3:2 or 2:1 resonance and start migrating outward (Masset & Snellgrove 2001;Pierens & Nelson 2008;Raymond et al 2011;Pierens et al 2014;Chametla et al 2020). We discuss, in Sect.…”

Section: Migration Mapsmentioning

confidence: 99%

Influence of planetary gas accretion on the shape and depth of gaps in protoplanetary discs

Bergez-Casalou

Bitsch

Pierens

et al. 2020

A&A

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It is widely known that giant planets have the capacity to open deep gaps in their natal gaseous protoplanetary discs. It is unclear, however, how gas accretion onto growing planets influences the shape and depth of their growing gaps. We performed isothermal hydrodynamical simulations with the Fargo-2D1D code, which assumes planets accreting gas within full discs that range from 0.1 to 260 AU. The gas accretion routine uses a sink cell approach, in which different accretion rates are used to cope with the broad range of gas accretion rates cited in the literature. We find that the planetary gas accretion rate increases for larger disc aspect ratios and greater viscosities. Our main results show that gas accretion has an important impact on the gap-opening mass: we find that when the disc responds slowly to a change in planetary mass (i.e., at low viscosity), the gap-opening mass scales with the planetary accretion rate, with a higher gas accretion rate resulting in a larger gap-opening mass. On the other hand, if the disc response time is short (i.e., at high viscosity), then gas accretion helps the planet carve a deep gap. As a consequence, higher planetary gas accretion rates result in smaller gap-opening masses. Our results have important implications for the derivation of planet masses from disc observations: depending on the planetary gas accretion rate, the derived masses from ALMA observations might be off by up to a factor of two. We discuss the consequences of the change in the gap-opening mass on the evolution of planetary systems based on the example of the grand tack scenario. Planetary gas accretion also impacts stellar gas accretion, where the influence is minimal due to the presence of a gas-accreting planet.

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“…Fig. 1 of Chametla et al (2020) shows two migration jumps in their model 7b in which a pair of Jupiter and Saturn (mass ratio 3:1) is migrating outwards in 3:2 MMR and experiences two small migration jumps between 5 and 8 au. This indicates, that migration jumps can also happen for other types of mean motion resonances, at smaller radii and for planet masses down to a pair of Jupiter and Saturn.…”

Section: Migration Jumpsmentioning

confidence: 99%

Migration jumps of planets in transition disks

Rometsch,

Rodenkirch,

Kley

et al. 2020

Preprint

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Context. Transition disks form a special class of protoplanetary disks that are characterized by a deficiency of disk material close to the star. In a subgroup, inner holes in these disks can stretch out to a few tens of au while there is still mass accretion onto the central star observed at the same time. Aims. We analyse the proposition that this type of wide transition disks is generated by the interaction of the disk with a system of embedded planets. Methods. We performed two-dimensional hydrodynamics simulations of a flat disk. Different equations of state were used including locally isothermal models and more realistic cases that consider viscous heating, radiative cooling and stellar heating. Two massive planets (with 3 to 9 Jupiter masses) were embedded in the disk and their dynamical evolution due to disk-planet interaction was followed for over 100 000 years. The simulations account for mass accretion onto the star and planets. We included models with parameters geared to the system PDS 70. To assess the observability of features in our models we performed synthetic ALMA observations. Results. For systems with a more massive inner planet, there are phases where both planets migrate outward engaged in a 2:1 mean motion resonance via the Masset-Snellgrove mechanism. In sufficiently massive disks the resulting formation of a vortex and the interaction with it can trigger rapid outward migration of the outer planet where its distance can increase by tens of au in a few thousand years. After another few thousand years, the outer planet rapidly migrates back inwards into resonance with the inner planet. We call this emerging composite phenomenon a migration jump. Outward migration and the migration jumps are accompanied by a high mass accretion rate onto the star. The synthetic images reveal numerous substructures depending on the type of dynamical behaviour. Conclusions. Our results suggest that the outward migration of two embedded planets is a prime candidate for the explanation of the observed high stellar mass accretion rate in wide transition disks. The models for PDS 70 indicate it does not currently undergo a migration jump but might very well be in a phase of outward migration. Key words. accretion, accretion disks -protoplanetary disks -planet-disk interactions -hydrodynamics -methods: numerical Consequently, it has been suggested early on that the presence of a massive (Jupiter-sized) planet might be responsible for the gap creation (Varnière et al. 2006;Rice et al. 2006), but at the same time it has been noticed that the gap created by a single embedded planet is significantly narrower than observations of Article number, page 1 of 21

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Capture and migration of Jupiter and Saturn in mean motion resonance in a gaseous protoplanetary disc

Cited by 14 publications

References 45 publications

Influence of planetary gas accretion on the shape and depth of gaps in protoplanetary discs

Influence of planetary gas accretion on the shape and depth of gaps in protoplanetary discs

Influence of planetary gas accretion on the shape and depth of gaps in protoplanetary discs

Migration jumps of planets in transition disks

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