Interpreting Brightness Asymmetries in Transition Disks: Vortex at Dead Zone or Planet-carved Gap Edges?

Regály, Zs.; Juhász, A.; Nehéz, Dóra

doi:10.3847/1538-4357/aa9a3f

Cited by 17 publications

(13 citation statements)

References 118 publications

(164 reference statements)

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“…We suggest two ways to distinguish them: First, planet-induced vortices frequently have off-center peaks due to repeated perturbations from the planet's spiral arms. On the contrary, Regály et al (2017) find that without these interactions, vortices at dead zone boundaries remain symmetric even when they have wide azimuthal extents.…”

Section: Confirmation Of Elongated Planet-induced Vorticesmentioning

confidence: 74%

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Observational diagnostics of elongated planet-induced vortices with realistic planet formation time-scales

Hammer

Pinilla

Kratter

et al. 2018

Monthly Notices of the Royal Astronomical Society

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Gap-opening planets can generate dust-trapping vortices that may explain some of the latest discoveries of high-contrast crescent-shaped dust asymmetries in transition discs. While planet-induced vortices were previously thought to have concentrated shapes, recent computational work has shown that these features naturally become much more elongated in the gas when simulations account for the relatively long timescale over which planets accrete their mass. In this work, we conduct two-fluid hydrodynamical simulations of vortices induced by slowly-growing Jupiter-mass planets in discs with very low viscosity (α = 3×10 −5 ). We simulate the dust dynamics for four particle sizes spanning 0.3 mm to 1 cm in order to produce synthetic ALMA images. In our simulations, we find that an elongated vortex still traps dust, but not directly at its center. With a flatter pressure bump and disruptions from the planet's overlapping spiral density waves, the dust instead circulates around the vortex. This motion (1) typically carries the peak off-center, (2) spreads the dust out over a wider azimuthal extent 180 • , (3) skews the azimuthal profile towards the front of the vortex, and (4) can also create double peaks in newly-formed vortices. In particular, we expect that the most defining observational signature, a peak offset of more than 30 • , should be detectable > 30% of the time in observations with a beam diameter of at most the planet's separation from its star.

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Section: Confirmation Of Elongated Planet-induced Vorticesmentioning

confidence: 74%

“…Second, Regály et al (2017) find that vortices at dead zone boundaries are much more radially-extended than those induced by rapidly-grown planets. In contrast, we have shown that elongated vortices have similar radial extents than concentrated vortices, providing another distinguishing criterion.…”

Section: Confirmation Of Elongated Planet-induced Vorticesmentioning

confidence: 89%

Observational diagnostics of elongated planet-induced vortices with realistic planet formation time-scales

Hammer

Pinilla

Kratter

et al. 2018

Monthly Notices of the Royal Astronomical Society

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“…We note that the lifetime of a vortex is difficult to predict. There are a number of factors that can reduce the lifetime of vortices, such as the viscosity (de Val-Borro et al 2007;Ataiee et al 2013;Fu et al 2014a;Regály et al 2017), dust feedback (Johansen et al 2004;Inaba & Barge 2006;Lyra et al 2009;Fu et al 2014b), disc self gravity (Regály & Vorobyov 2017a;Pierens & Lin 2018) and the streaming instability (Raettig et al 2015). The lifetimes of vortices formed by giant planets has been investigated and were found to be strongly dependent on planet mass and viscosity, capable of sustaining vortices up to 10 4 orbits in some cases (Fu et al 2014a).…”

Section: Discussionmentioning

confidence: 99%

Constraining the masses of planets in protoplanetary discs from the presence or absence of vortices – comparison with ALMA observations

Hallam

Paardekooper

2019

Monthly Notices of the Royal Astronomical Society

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A massive planet in a protoplanetary disc will open a gap in the disc material. A steep gap edge can be hydrodynamically unstable, which results in the formation of vortices that can act as tracers for the presence of planets in observational results. However, in a viscous disc, the potential formation of these vortices is dependent on the timescale over which the massive planet accretes mass and with a sufficiently long timescale it is possible for no vortices to form. Hence, there is a connection between the presence of vortices and the growth timescale of the planet and it may therefore be possible to exclude a planetary interpretation of observed structure from the absence of vortices. We have investigated the effect of the planet growth timescale on vortex formation for a range of planet masses and viscosities and have found an approximate relation between the planet mass, viscosity and planet growth timescale for which vortices are not formed within the disc. We then interpret these results in the light of recent observations. We have also found that planets do not need to be close to a Jupiter mass to form vortices in the disc if these discs have low viscosity, as these can be caused by planets as small as a few Neptune masses.

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“…For instance, observations from the near-infrared to millimeter bands in dust continuum and in scattered light have revealed a variety of disk substructures, such as spiral arcs and arms, clumps, rings, and gaps (e.g., van der Marel et al 2013; ALMA Partnership et al 2015;Pérez et al 2016;Liu et al 2016), indicating that protoplanetary disks often do not have simple monotonically declining surface density profiles. Theoretical interpretations of these substructures imply a presence of already-formed massive planets (e.g., Kley & Nelson 2012) or/and physical phenomena at work, such as gravitational instability or vortices, which can assist planet formation (e.g., Dong et al 2016;Regály et al 2017).…”

Section: Introductionmentioning

confidence: 99%

The origin of tail-like structures around protoplanetary disks

Vorobyov

Skliarevskii

Elbakyan

et al. 2020

A&A

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Aims. We study the origin of tail-like structures recently detected around the disk of SU Aurigae and several FU Orionis type stars. Methods. Dynamic protostellar disks featuring ejections of gaseous clumps and quiescent protoplanetary disks experiencing a close encounter with an intruder star were modelled using the numerical hydrodynamics code FEOSAD. Both the gas and dust dynamics were taken into account, including dust growth and mutual friction between the gas and dust components. Only plane-of-the-disk encounters were considered. Results. Ejected clumps produce a unique type of tails that are characterized by a bow-shock shape. These tails owe its origin to the supersonic motion of the ejected clumps through the dense envelope, which often surrounds young gravitationally unstable protostellar disks. The ejected clumps either sit at the head of the tail-like structure or disperse if their mass is insufficient to withstand the head wind of the envelope. On the other hand, close encounters with quiescent protoplanetary disks produce three types of the tail-like structures, which we defined as pre-collisional, post-collisional, and spiral tails. These tails can in principle be distinguished by peculiar features of the gas and dust flow in and around them. We found that the brown-dwarf-mass intruders do not capture circumintruder disks during the encounter, while the sub-solar-mass intruders can acquire appreciable circumintruder disks with elevated dust-to-gas ratios, which can ease their observational detection. However, this is true only for prograde collisions; the retrograde intruders fail to collect an appreciable gas and dust from the disk of the target. The masses of gas in the tails vary in the 0.85-11.8 M Jup limits, while the total mass of dust lies in the 1.75-30.1 M ⊕ range, with the spiral tails featuring the highest masses. The predicted mass of dust in the model tail-like structures is therefore higher than what was inferred for similar structures in SU Aur, FU Ori, and Z CMa, making their observational detection feasible. Conclusions. Tail-like structures around protostellar and protoplanetary disks can act as a smoking gun to infer interesting phenomena, such as clump ejection or close encounters. particular, the bow-shock morphology of the tails could point to clump ejections as a possible formation mechanism. Further numerical and observational studies are needed to better understand the detectability and properties of the tails.

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Interpreting Brightness Asymmetries in Transition Disks: Vortex at Dead Zone or Planet-carved Gap Edges?

Cited by 17 publications

References 118 publications

Observational diagnostics of elongated planet-induced vortices with realistic planet formation time-scales

Observational diagnostics of elongated planet-induced vortices with realistic planet formation time-scales

Constraining the masses of planets in protoplanetary discs from the presence or absence of vortices – comparison with ALMA observations

The origin of tail-like structures around protoplanetary disks

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