Three‐dimensional Interaction between a Planet and an Isothermal Gaseous Disk. I. Corotation and Lindblad Torques and Planet Migration

Tanaka, Hidekazu; Takeuchi, Taku; Ward, William R.

doi:10.1086/324713

Cited by 987 publications

(1,426 citation statements)

References 24 publications

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“…3 the specific torques (in absolute value) obtained with the fixed and free cases, for a h = 0.05 disk aspect ratio. In the fixed situation, there is an excellent agreement with the expectation γ ∝ Σ p , and, not surprisingly, the torques are bounded by the two-and three-dimensional analytical estimates of Tanaka et al (2002). Nonetheless, the free case reveals two unexpected results.…”

Section: Case Of a Non Self-gravitating Disksupporting

confidence: 60%

“…This is the configuration that has been contemplated in analytical torque estimates (see e.g. Tanaka et al 2002).…”

Section: Case Of a Non Self-gravitating Diskmentioning

confidence: 99%

“…(25) therefore reads (Γ fsg − Γ asg+ap )/Γ C,asg . The quantity Γ C,asg can be connected with Γ asg , using the estimate of Tanaka et al (2002) for a flat surface density profile. This connection is motivated by the fact that both the differential Lindblad torque, and the corotation torque are almost identical in the nog and asg situations.…”

Section: Corotation Torque Issuesmentioning

confidence: 99%

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Type I planetary migration in a self-gravitating disk

Masset

2007

Proc. IAU

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We investigate the tidal interaction between a low-mass planet and a selfgravitating protoplanetary disk, by means of two-dimensional hydrodynamic simulations. We first show that considering a planet freely migrating in a disk without self-gravity leads to a significant overestimate of the migration rate. The overestimate can reach a factor of two for a disk having three times the surface density of the minimum mass solar nebula. Unbiased drift rates may be obtained only by considering a planet and a disk orbiting within the same gravitational potential. In a second part, the disk self-gravity is taken into account. We confirm that the disk gravity enhances the differential Lindblad torque with respect to the situation where neither the planet nor the disk feels the disk gravity. This enhancement only depends on the Toomre parameter at the planet location. It is typically one order of magnitude smaller than the spurious one induced by assuming a planet migrating in a disk without self-gravity. We confirm that the torque enhancement due to the disk gravity can be entirely accounted for by a shift of Lindblad resonances, and can be reproduced by the use of an anisotropic pressure tensor. We do not find any significant impact of the disk gravity on the corotation torque.Subject headings: accretion, accretion disks -hydrodynamics -methods: numerical -planetary systems: formation -planetary systems: protoplanetary disks 1 Send offprint requests to clement.baruteau@cea.fr.

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Section: Case Of a Non Self-gravitating Disksupporting

confidence: 60%

“…This is the configuration that has been contemplated in analytical torque estimates (see e.g. Tanaka et al 2002).…”

Section: Case Of a Non Self-gravitating Diskmentioning

confidence: 99%

Section: Corotation Torque Issuesmentioning

confidence: 99%

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Type I planetary migration in a self-gravitating disk

Masset

2007

Proc. IAU

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“…As large dust concentrates in the vortex centre, we take a shallower size distribution within the affected size range as explained in Lyra & Lin (2013). Planet-induced spirals (Tanaka et al 2002) are expected in protoplanetary discs and both the contribution of the planet and the spirals could end up in the astrometric measurements. Gravitational instabilities may develop in protoplanetary discs and lead to fragmentation and clump formation (e.g.…”

Section: -Inhomogeneties In Protoplanetary Discmentioning

confidence: 99%

Effects of disc asymmetries on astrometric measurements

Kral

Kennedy

Souami

2016

A&A

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Astrometry covers a parameter space that cannot be reached by RV or transit methods to detect terrestrial planets on wide orbits. In addition, high accuracy astrometric measurements are necessary to measure the inclination of the planet's orbits. Here we investigate the principles of an artefact of the astrometric approach, namely the displacement of the photo-centre owing to inhomogeneities in a dust disc around the parent star. Indeed, theory and observations show that circumstellar discs can present strong asymmetries. We model the pseudo-astrometric signal caused by these inhomogeneities, asking whether a dust clump in a disc can mimic the astrometric signal of an Earth-like planet. We show that these inhomogeneities cannot be neglected when using astrometry to find terrestrial planets. We provide the parameter space for which these inhomogeneities can affect the astrometric signals but still not be detected by mid-IR observations. We find that a small cross section of dust corresponding to a cometary mass object is enough to mimic the astrometric signal of an Earth-like planet. Astrometric observations of protoplanetary discs to search for planets can also be affected by the presence of inhomogeneities. Some further tests are given to confirm whether an observation is a real astrometric signal from a planet or an impostor. Eventually, we also study the case where the cross-section of dust is high enough to provide a detectable IR-excess and to have a measurable photometric displacement by actual instruments such as Gaia, IRAC, or GRAVITY. We suggest a new method, which consists of using astrometry to quantify asymmetries (clumpiness) in inner debris discs that cannot be otherwise resolved.

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“…Most of the Kepler candidate planets are sufficiently small that they are unable to open gaps in the protoplanetary disks and should undergo type I migration. For classic type I migration, the migration and eccentricity damping timescales are (Ward 1997;Tanaka et al 2002;Artymowicz 1993)…”

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confidence: 99%

Evidence for Solid Planets from Kepler's Near-Resonance Systems

2012

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Abstract. The multiple-planet systems discovered by the Kepler mission show an excess of planet pairs with period ratios just wide of exact commensurability for first-order resonances like 2:1 and 3:2. In principle, these planet pairs could be in resonance if their orbital eccentricities are sufficiently small, because the width of first-order resonances diverges in the limit of vanishingly small eccentricity. We consider a widely-held scenario in which pairs of planets were captured into first-order resonances by migration due to planet-disk interactions, and subsequently became detached from the resonances, due to tidal dissipation in the planets. In the context of this scenario, we find a constraint on the ratio of the planet's tidal dissipation function and Love number that implies that some of the Kepler planets are likely solid. However, tides are not strong enough to move many of the planet pairs to the observed separations, suggesting that additional processes are at play.

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Three‐dimensional Interaction between a Planet and an Isothermal Gaseous Disk. I. Corotation and Lindblad Torques and Planet Migration

Cited by 987 publications

References 24 publications

Type I planetary migration in a self-gravitating disk

Type I planetary migration in a self-gravitating disk

Effects of disc asymmetries on astrometric measurements

Evidence for Solid Planets from Kepler's Near-Resonance Systems

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