Toward a new paradigm for Type II migration

Robert, Carmelle; Crida, A.; Lega, Elena; Méheut, H.; Morbidelli, Alessandro

doi:10.1051/0004-6361/201833539

Cited by 72 publications

(62 citation statements)

References 28 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The closest work to the one we present here is Robert et al (2018). These authors showed that the migration rate scales with the viscosity, as expected in type II migration.…”

Section: Comparison With Previous Work: Type II Migration Is Correct supporting

confidence: 77%

“…Lastly, it should be noted that, although mass transport through the gap does happen, it is not the reason for the apparent discrepancy from type II migration. Robert et al (2018) showed that one obtains similar migration rates also when cutting the mass transport through the gap. Along the same lines, our simulations show that the mass transport through the gap decreases with time and eventually becomes smaller than the viscous rate.…”

Section: Comparison With Previous Work: Type II Migration Is Correct mentioning

confidence: 91%

See 1 more Smart Citation

Type II migration strikes back – an old paradigm for planet migration in discs

Scardoni

Rosotti

Lodato

et al. 2019

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

In this paper we analyse giant gap-opening planet migration in protoplanetary discs, focusing on the type II migration regime. According to standard type II theory, planets migrate at the same rate as the gas in the disc, as they are coupled to the disc viscous evolution; however, recent studies questioned this paradigm, suggesting that planets migrate faster than the disc material. We study the problem through 2D long-time simulations of systems consistent with type II regime, using the hydrodynamical grid code FARGO3D. Even though our simulations confirm the presence of an initial phase characterised by fast migration, they also reveal that the migration velocity slows down and eventually reaches the theoretical prediction if we allow the system to evolve for enough time. We find the same tendency to evolve towards the theoretical predictions at later times when we analyse the mass flow through the gap and the torques acting on the planet. This transient is related to the initial conditions of our (and previous) simulations, and is due to the fact that the shape of the gap has to adjust to a new profile, once the planet is set into motion. Secondly, we test whether the type II theory expectation that giant planet migration is driven by viscosity is consistent with our simulation by comparing simulations with the same viscosity and different disc mass (or viceversa). We find a good agreement with the theory, since when the discs are characterised by the same viscosity, the migration properties are the same.

show abstract

“…The closest work to the one we present here is Robert et al (2018). These authors showed that the migration rate scales with the viscosity, as expected in type II migration.…”

Section: Comparison With Previous Work: Type II Migration Is Correct supporting

confidence: 77%

Section: Comparison With Previous Work: Type II Migration Is Correct mentioning

confidence: 91%

Type II migration strikes back – an old paradigm for planet migration in discs

Scardoni

Rosotti

Lodato

et al. 2019

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…This function is based on Robert et al (2018), where the authors assume that close to the planet gas accretion is 100% efficient ( f red = 1). However, it seems that 100% efficiency is not realistic in such a case.…”

Section: The Fargo-2d1d Codementioning

confidence: 99%

“…The main motivation for these studies has, in fact, been the migration of the giant planets that have the capacity to open these deep gaps. However, it is only recently that these migration studies have started to factor in planetary gas accretion (Dürmann & Kley 2015;Crida & Bitsch 2017;Robert et al 2018).…”

Section: Introductionmentioning

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

Self Cite

View full text Add to dashboard Cite

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.

show abstract

“…This would result in a decoupled planetary migration that can differ from the viscous accretion speed (Duffell et al 2014;Dürmann & Kley 2015). Simulations can even have a planet migrating through a stationary disk (Robert et al 2018).…”

Section: Classic Type II Migrationmentioning

confidence: 99%

Inflation of migrated hot Jupiters

Lous

Miguel

2020

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

The observed low densities of gas giant planets with a high equilibrium temperature (hot Jupiters) can be simulated in models when a fraction of the surface radiation is deposited deeper in the interior. Meanwhile, migration theories suggest that hot Jupiters formed further away from their host star and migrated inward. We incorporate disc migration in simulations of the evolving interior of hot Jupiters to determine whether migration has a long-lasting effect on the inflation of planets. We quantify the difference between the radius of a migrated planet and the radius of a planet that formed in situ as the radius discrepancy. We remain agnostic about the physical mechanism behind interior heating, but assume it scales with the received stellar flux by a certain fraction. We find that the change in irradiation received from the host star while the planet is migrating can affect the inflation and final radius of the planet. Models with a high fraction of energy deposited in the interior (>5 per cent) show a significant radius discrepancy when the deposit is at higher pressures than $P=1 \, \mathrm{bar}$. For a smaller fraction of 1 per cent, there is no radius discrepancy for any deposit depth. We show that a uniform heating mechanism can cause different rates of inflation, depending on the migration history. If the forthcoming observations on mean densities and atmospheres of gas giants give a better indication of a potential heating mechanism, this could help to constrain the prior migration of such planets.

show abstract

Toward a new paradigm for Type II migration

Cited by 72 publications

References 28 publications

Type II migration strikes back – an old paradigm for planet migration in discs

Type II migration strikes back – an old paradigm for planet migration in discs

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

Inflation of migrated hot Jupiters

Contact Info

Product

Resources

About