Observable scattered light features from inclined and non-inclined planets embedded in protoplanetary discs

Kloster, Dylan; Flock, Mario

doi:10.1093/mnras/stz1649

Cited by 4 publications

(2 citation statements)

References 70 publications

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“…The planet is fixed on a circular and coplanar orbit with R p = 1 in code units. A moderate inclination that keeps the planet within the disk (i h, where h is the disk aspect ratio) is unlikely to enhance spiral temperature structures as strongly as it does scattered light (e.g., Kloster & Flock 2019), although more substantial inclination would diminish the planet's ability to transmit angular momentum to the disk and consequently reduce spiral visibility. We leave a detailed study on the effect of inclination to future work.…”

Section: Methodsmentioning

confidence: 99%

Observational Signatures of Planets in Protoplanetary Disks: Temperature structures in spiral arms

Muley,

Dong,

Fung

2021

Preprint

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High-resolution imaging of protoplanetary disks has unveiled a rich diversity of spiral structure, some of which may arise from disk-planet interaction. Using 3D hydrodynamics with β-cooling to a vertically stratified background, as well as radiative-transfer modeling, we investigate the temperature rise in planet-driven spirals. In rapidly cooling disks, the temperature rise is dominated by a contribution from stellar irradiation, 0.3-3% inside the planet radius but always < 0.5% outside. When cooling time equals or exceeds dynamical time, however, this is overwhelmed by hydrodynamic P dV work, which introduces a ∼10 − 20% perturbation within a factor of ∼ 2 from the planet's orbital radius. We devise an empirical fit of the spiral amplitude ∆(T ) = (M p /M th ) c (f P dV e −tarm/tc + f rad ) to take into account both effects. Where cooling is slow, we find also that temperature perturbations from buoyancy spirals -a strictly 3D, non-isothermal phenomenon -become nearly as strong as those from Lindblad spirals, which are amenable to 2D and isothermal studies. Our findings may help explain observed thermal features in disks like TW Hydrae and CQ Tauri, and underscore that 3D effects have a qualitatively important effect on disk structure.

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Section: Methodsmentioning

confidence: 99%

Observational Signatures of Planets in Protoplanetary Disks: Temperature structures in spiral arms

Muley,

Dong,

Fung

2021

Preprint

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“…Focusing on the features created by planets, it is hard to observe the planets directly while they are embedded in their protoplanetary disk (Sanchis et al 2020;Kloster & Flock 2019;Asensio-Torres et al 2021). Therefore, analyzing the dust gap size (Zhang et al 2018) or the CO velocity perturbations (Teague et al 2018;Pinte et al 2020) are ways to indirectly derive the properties of potentially embedded planets.…”

Section: Introductionmentioning

confidence: 99%

Constraining giant planet formation with synthetic ALMA images of the Solar System’s natal protoplanetary disk

Bergez-Casalou

Bitsch

Kurtovic

et al. 2022

A&A

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New ALMA observations of protoplanetary disks allow us to probe planet formation in other planetary systems, giving us new constraints on planet formation processes. Meanwhile, studies of our own Solar System rely on constraints derived in a completely different way. However, it is still unclear what features the Solar System protoplanetary disk could have produced during its gas phase. By running 2D isothermal hydro-simulations used as inputs for a dust evolution model, we derive synthetic images at millimeter wavelengths using the radiative transfer code RADMC3D. We find that the embedded multiple giant planets strongly perturb the radial gas velocities of the disk. These velocity perturbations create traffic jams in the dust, producing over-densities different from the ones created by pressure traps and located away from the planets’ positions in the disk. By deriving the images at λ = 1.3 mm from these dust distributions, we show that very high resolution observations are needed to distinguish the most important features expected in the inner part (<15 AU) of the disk. The traffic jams, observable with a high resolution, further blur the link between the number of gaps and rings in disks and the number of embedded planets. We additionally show that a system capable of producing eccentric planets by scattering events that match the eccentricity distributions in observed exoplanets does not automatically produce bright outer rings at large radii in the disk. This means that high resolution observations of disks of various sizes are needed to distinguish between different giant planet formation scenarios during the disk phase, where the giants form either in the outer regions of the disks or in the inner regions. In the second scenario, the disks do not present planet-related features at large radii. Finally, we find that, even when the dust temperature is determined self-consistently, the dust masses derived observationally might be off by up to a factor of ten compared to the dust contained in our simulations due to the creation of optically thick regions. Our study clearly shows that in addition to the constraints from exoplanets and the Solar System, ALMA has the power to constrain different stages of planet formation already during the first few million years, which corresponds to the gas disk phase.

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Kinematic signatures of a low-mass planet with a moderately inclined orbit in a protoplanetary disk

Kanagawa,

Ono,

Momose

2023

Publications of the Astronomical Society of Japan

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A planet embedded in a protoplanetary disk produces a gap by disk–planet interaction. It also generates velocity perturbation of gas, which can also be observed as deviations from the Keplerian rotation in the channel map of molecular line emission, called kinematic planetary features. These observed signatures provide clues to determine the mass of the planet. We investigated the features induced by a planet with an inclined orbit through three-dimensional hydrodynamic simulations. We found that a smaller planet, with an inclination of ∼10○–20○, can produce kinematic features as prominent as those induced by a massive coplanar planet. Despite the kinematic features being similar, the gap is shallower and narrower compared with the case in which the kinematic features are formed by a coplanar planet. We also found that the kinematic features induced by an inclined planet were fainter for rarer CO isotopologues because the velocity perturbation is weaker at the position closer to the midplane, which was different in the case with a coplanar massive planet. This dependence on the isotopologues is distinguished if the planet has an inclined orbit. We discussed two observed kinematic features in the disk of HD 163296. We concluded that the kink observed at 220 au can be induced by an inclined planet, while the kink at 67 au is consistent to that induced by a coplanar planet.

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Observable scattered light features from inclined and non-inclined planets embedded in protoplanetary discs

Cited by 4 publications

References 70 publications

Observational Signatures of Planets in Protoplanetary Disks: Temperature structures in spiral arms

Observational Signatures of Planets in Protoplanetary Disks: Temperature structures in spiral arms

Constraining giant planet formation with synthetic ALMA images of the Solar System’s natal protoplanetary disk

Kinematic signatures of a low-mass planet with a moderately inclined orbit in a protoplanetary disk

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