Evolution of Giant Planets in Eccentric Disks

D’Angelo, Gennaro; Lubow, Stephen H.; Bate, Matthew R.

doi:10.1086/508451

Cited by 158 publications

(129 citation statements)

References 53 publications

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“…It shows a clear elliptic character of the gap opened by the giant planet. According to Kley & Dirksen (2006), D'Angelo et al (2006), and also to our calculations (see below), the disk becomes eccentric after several hundred orbits of the embedded planet. With regard to our synthetic spectral line model, the most relevant are those effects that are originating from the gas dynamics caused by the giant planet.…”

Section: Disk Modelssupporting

confidence: 75%

Detectability of giant planets in protoplanetary disks by CO emission lines

Regály

Sándor

Dullemond

et al. 2010

A&A

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Context. Planets are thought to form in protoplanetary accretion disks around young stars. Detecting a giant planet still embedded in a protoplanetary disk would be very important and give observational constraints on the planet-formation process. However, detecting these planets with the radial velocity technique is problematic owing to the strong stellar activity of these young objects. Aims. We intend to provide an indirect method to detect Jovian planets by studying near infrared emission spectra originating in the protoplanetary disks around T Tauri stars. Our idea is to investigate whether a massive planet could induce any observable effect on the spectral lines emerging in the disks atmosphere. As a tracer molecule we propose CO, which is excited in the ro-vibrational fundamental band in the disk atmosphere to a distance of ∼2−3 AU (depending on the stellar mass) where terrestrial planets are thought to form. Methods. We developed a semi-analytical model to calculate synthetic molecular spectral line profiles in a protoplanetary disk using a double layer disk model heated on the outside by irradiation by the central star and in the midplane by viscous dissipation due to accretion. 2D gas dynamics were incorporated in the calculation of synthetic spectral lines. The motions of gas parcels were calculated by the publicly available hydrodynamical code FARGO which was developed to study planet-disk interactions. Results. We demonstrate that a massive planet embedded in a protoplanetary disk strongly influences the originally circular Keplerian gas dynamics. The perturbed motion of the gas can be detected by comparing the CO line profiles in emission, which emerge from planet-bearing to those of planet-free disk models. The planet signal has two major characteristics: a permanent line profile asymmetry, and short timescale variability correlated with the orbital phase of the giant planet. We have found that the strength of the asymmetry depends on the physical parameters of the star-planet-disk system, such as the disk inclination angle, the planetary and stellar masses, the orbital distance, and the size of the disk inner cavity. The permanent line profile asymmetry is caused by a disk in an eccentric state in the gap opened by the giant planet. However, the variable component is a consequence of the local dynamical perturbation by the orbiting giant planet. We show that a forming giant planet, still embedded in the protoplanetary disk, can be detected using contemporary or future high-resolution near-IR spectrographs like VLT/CRIRES and ELT/METIS.

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Section: Disk Modelssupporting

confidence: 75%

Detectability of giant planets in protoplanetary disks by CO emission lines

Regály

Sándor

Dullemond

et al. 2010

A&A

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“…These correlations, if related to the formation processes, may give important indications about the origin of high eccentricities. Many theories have been proposed (Holman et al 1997;Murray et al 2002;Goldreich & Sari 2003;Zakamska & Tremaine 2004;Namouni 2005;Adams & Laughlin 2006;D'Angelo et al 2006;Fregeau et al 2006), but none has observational support yet. Here we suggest that the metallicity acts in some way in determining e. For instance, since high [ Fe/H] produces a faster migration, the low values of e observed for high [ Fe/H] may be the result of the migration process, e.g., tidal circularization (see also Halbwachs et al 2005).…”

Section: Cluster C3mentioning

confidence: 99%

Extrasolar Planet Taxonomy: A New Statistical Approach

Marchi

2007

ApJ

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In this paper we present the guidelines for an extrasolar planet taxonomy. The discovery of an increasing number of extrasolar planets showing a vast variety of planetary parameters, such as Keplerian orbital elements, and environmental parameters, such as stellar masses, spectral types, and metallicity, prompts the development of a planetary taxonomy. In this work, via principal component analysis followed by hierarchical clustering analysis, we report the definition of five robust groups of planets. We also discuss the physical relevance of such analysis, which may provide a valid basis for disentangling the role of the several physical parameters involved in the processes of planet formation and subsequent evolution. For instance, we were able to divide the hot Jupiters into two main groups on the basis of their stellar masses and metallicities. Moreover, for some groups, we find strong correlations among metallicity, semimajor axis, and eccentricity. The implications of these findings are discussed.

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“…In turn, this eccentric disc can possibly increase the planetary eccentricity (Papaloizou et al 2001;D'Angelo et al 2006). However, this process can only explain the eccentricity of very massive (≈5-10 M Jup ) planets.…”

Section: Introductionmentioning

confidence: 99%

Highly inclined and eccentric massive planets

Bitsch

Crida

Libert

et al. 2013

A&A

122

188

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Context. In the solar system, planets have a small inclination with respect to the equatorial plane of the Sun, but there is evidence that in extrasolar systems the inclination can be very high. This spin-orbit misalignment is unexpected, as planets form in a protoplanetary disc supposedly aligned with the stellar spin. It has been proposed that planet-planet interactions can lead to mutual inclinations during migration in the protoplanetary disc. However, the effect of the gas disc on inclined giant planets is still unknown. Aims. In this paper we investigate planet-disc interactions for planets above 1 M Jup . We check the influence of three parameters: the inclination i, eccentricity e, and mass M p of the planet. This analysis also aims at providing a general expression of the eccentricity and inclination damping exerted on the planet by the disc. Methods. We perform three-dimensional numerical simulations of protoplanetary discs with embedded high-mass planets on fixed orbits. We use the explicit/implicit hydrodynamical code NIRVANA in 3D with an isothermal equation of state. Results. We provide damping formulae for i and e as a function of i, e, and M p that fit the numerical data. For highly inclined massive planets, the gap opening is reduced, and the damping of i occurs on time-scales of the order of 10 −4 deg/year · M disc /(0.01 M ) with the damping of e on a smaller time-scale. While the inclination of low planetary masses (<5 M Jup ) is always damped, large planetary masses with large i can undergo a Kozai-cycle with the disc. These Kozai-cycles are damped through the disc in time. Eccentricity is generally damped, except for very massive planets (M p ∼ 5 M Jup ) where eccentricity can increase for low inclinations. So the dynamics tends to a final state: planets end up in midplane and can then, over time, increase their eccentricity as a result of interactions with the disc. Conclusions. The interactions with the disc lead to damping of i and e after a scattering event of high-mass planets. If i is sufficiently reduced, the eccentricity can be pumped up because of interactions with the disc. If the planet is scattered to high inclination, it can undergo a Kozai-cycle with the disc that makes it hard to predict the exact movement of the planet and its orbital parameters at the dispersal of the disc.

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Evolution of Giant Planets in Eccentric Disks

Cited by 158 publications

References 53 publications

Detectability of giant planets in protoplanetary disks by CO emission lines

Detectability of giant planets in protoplanetary disks by CO emission lines

Extrasolar Planet Taxonomy: A New Statistical Approach

Highly inclined and eccentric massive planets

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