Debris Disks in Multiplanet Systems: Are Our Inferences Compromised by Unseen Planets?

Dong, Jiayin; Dawson, Rebekah I.; Shannon, Andrew; Morrison, Sarah J.

doi:10.3847/1538-4357/ab64f7

Cited by 11 publications

(9 citation statements)

References 80 publications

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“…A planet exterior to the parent belt on an inclined orbit could also, by a combination of warping and orbital precession, vertically thicken the belt, but here again the time-scales are of the order of several Myrs (Dong et al 2020 ), highly exceeding the gas-induced settling time that we observe in our model.…”

Section: Planet Induced Vertical Stirringmentioning

confidence: 47%

The vertical structure of debris discs and the impact of gas

Olofsson

Thébault

Kral

et al. 2022

Monthly Notices of the Royal Astronomical Society

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The vertical structure of debris disks provides clues about their dynamical evolution and the collision rate of the unseen planetesimals. Thanks to the ever-increasing angular resolution of contemporary instruments and facilities, we are beginning to constrain the scale height of a handful of debris disks, either at near-infrared or millimeter wavelengths. Nonetheless, this is often done for individual targets only. We present here the geometric modeling of eight disks close to edge-on, all observed with the same instrument (SPHERE) and using the same mode (dual-beam polarimetric imaging). Motivated by the presence of CO gas in two out of the eight disks, we then investigate the impact that gas can have on the scale height by performing N-body simulations including gas drag and collisions. We show that gas can quickly alter the dynamics of particles (both in the radial and vertical directions), otherwise governed by gravity and radiation pressure. We find that, in the presence of gas, particles smaller than a few tens of microns can efficiently settle toward the midplane at the same time as they migrate outward beyond the birth ring. For second generation gas (Mgas ≤ 0.1 M⊕), the vertical settling should be best observed in scattered light images compared to observations at millimeter wavelengths. But if the gas has a primordial origin (Mgas ≥ 1 M⊕), the disk will appear very flat both at near-infrared and sub-mm wavelengths. Finally, far beyond the birth ring, our results suggest that the surface brightness profile can be as shallow as ∼−2.25.

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Section: Planet Induced Vertical Stirringmentioning

confidence: 47%

The vertical structure of debris discs and the impact of gas

Olofsson

Thébault

Kral

et al. 2022

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…A planet exterior to the parent belt on an inclined orbit could also, by a combination of warping and orbital precession, vertically thicken the belt, but here again the timescales are of the order of several Myrs (Dong et al 2020), highly exceeding the gas-induced settling time that we observe in our model.…”

Section: Planet Induced Vertical Stirringmentioning

confidence: 48%

The vertical structure of debris disks and the impact of gas

Olofsson,

Thébault,

Kral

et al. 2022

Preprint

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The vertical structure of debris disks provides clues about their dynamical evolution and the collision rate of the unseen planetesimals. Thanks to the ever-increasing angular resolution of contemporary instruments and facilities, we are beginning to constrain the scale height of a handful of debris disks, either at near-infrared or millimeter wavelengths. Nonetheless, this is often done for individual targets only. We present here the geometric modeling of eight disks close to edge-on, all observed with the same instrument (SPHERE) and using the same mode (dual-beam polarimetric imaging). Motivated by the presence of CO gas in two out of the eight disks, we then investigate the impact that gas can have on the scale height by performing N-body simulations including gas drag and collisions. We show that gas can quickly alter the dynamics of particles (both in the radial and vertical directions), otherwise governed by gravity and radiation pressure. We find that, in the presence of gas, particles smaller than a few tens of microns can efficiently settle toward the midplane at the same time as they migrate outward beyond the birth ring. For second generation gas (𝑀 gas ≤ 0.1 𝑀 ⊕ ), the vertical settling should be best observed in scattered light images compared to observations at millimeter wavelengths. But if the gas has a primordial origin (𝑀 gas ≥ 1 𝑀 ⊕ ), the disk will appear very flat both at near-infrared and sub-mm wavelengths. Finally, far beyond the birth ring, our results suggest that the surface brightness profile can be as shallow as ∼ −2.25.

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“…Compiling the spectral energy distributions (SEDs) of the 162 perturbers of all the systems that caused close encounters within the last 5 Myr, we find that 25% of all of them do show a FIR excess over the stellar photosphere. Since the orbital change of planetesimal (e.g., eccentricity and inclination) can result from the existence of nearby sculpting planet through close encounters (Larwood & Kalas 2001;Kalas et al 2007;Dong et al 2020), possibly leading to the change of disk's vertical scale height (Quillen et al 2007); this could be a signature of debris material around the central star.…”

Section: Resultsmentioning

confidence: 99%

Flybys in debris disk systems withGaiaeDR3

Bertini

Roccatagliata

Kim

2023

A&A

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Context. Debris disks represent the last phase of the evolution of protoplanetary disks around young stellar objects where planetary systems had most likely already been formed. Resolved systems show peculiar structures, such as asymmetries or spirals, which may be associated with either the presence of a low-mass companion or dynamical interactions with a perturber during a flyby event.Aims. We aim to observationally and statistically constrain the influence of flybys in the formation and evolution of debris disks. Methods. We compiled a sample of 254 debris disks with ages between 2 Myr and 8 Gyr that are either part of an association or isolated, drawing the binary and planetary companions of the systems mainly from the literature. Using the Gaia eDR3 astrometric data and radial velocities of our sample, as well as all the sources in a specific region of the sky, we reconstructed the relative linear motions in the last 5 Myr and made predictions for the next 2 Myr. Relating the Hill radius of each debris disk system and the closest distances reached by the two sources, we defined the flyby events in terms of position and time.Results. We find that in the period between the last 5 Myrs and the next 2 Myrs, 90% of the analyzed systems have experienced at least a close flyby, while 7% of them have experienced flybys at distances greater than 0.5R Hill . In particular, 75% of them have experienced at least one past close encounter and 36% multiple past close encounters. From the sub-sample of resolved debris disk (41 out of 94), 80% of the analyzed systems experience at least an encounter within 0.8 pc. From the subsample of 10 debris disks with planets, half of these systems do show misalignments between disk and planet, stirring, or asymmetries. Systems with a misalignment between the planetary orbit and the disk do indeed experience at least one flyby event. In particular, when the planet orbits have a difference with the disk inclination higher than about 20 • , as in the case of HD 38529, we find that multiple close encounters have taken place in the last 5 Myr, as theoretically predicted. Conclusions. The high incidence of encounters, particularly close encounters, experienced by the systems in the last 5 Myr suggests the fundamental impact of flybys on the evolution of debris disks. Moreover, despite the low statistics, it is interesting to highlight that flybys that have been theoretically predicted so far in peculiar resolved systems have also been observationally constrained.

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Debris Disks in Multiplanet Systems: Are Our Inferences Compromised by Unseen Planets?

Cited by 11 publications

References 80 publications

The vertical structure of debris discs and the impact of gas

The vertical structure of debris discs and the impact of gas

The vertical structure of debris disks and the impact of gas

Flybys in debris disk systems withGaiaeDR3

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