Inclined massive planets in a protoplanetary disc: gap opening, disc breaking, and observational signatures

Zhu, Zhaohuan

doi:10.1093/mnras/sty3358

Cited by 88 publications

(59 citation statements)

References 107 publications

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“…Nazari et al (2019) showed that the number and shape of gaps depend on the migration speed of a planet and the drift speed of dust. Also, increasing an inclination angle of the planet orbit relative to the disk midplane tends to make a gap shallower (Zhu 2018).…”

Section: Discussionmentioning

confidence: 99%

Properties of Density and Velocity Gaps Induced by a Planet in a Protoplanetary Disk

Yun

Kim

Bae

et al. 2019

ApJ

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Gravitational interactions between a protoplanetary disk and its embedded planet is one of the formation mechanisms of gaps and rings found in recent ALMA observations. To quantify the gap properties measured in not only surface density but also rotational velocity profiles, we run twodimensional hydrodynamic simulations of protoplanetary disks by varying three parameters: the mass ratio q of a planet to a central star, the ratio of the disk scale height h p to the orbital radius r p of the planet, and the viscosity parameter α. We find the gap depth δ Σ in the gas surface density depends on a single dimensionless parameter K ≡ q 2 (h p /r p ) −5 α −1 as δ Σ = (1 + 0.046K) −1 , consistent with the previous results of Kanagawa et al. (2015a). The gap depth δ V in the rotational velocity is given by δ V = 0.007(h p /r p )K 1.38 /(1 + 0.06K 1.03 ). The gap width, in both surface density and rotational velocity, has a minimum of about 4.7h p when the planet mass M p is around the disk thermal mass M th , while it increases in a power-law fashion as M p /M th increases or decrease from unity. Such a minimum in the gap width arises because spirals from sub-thermal planets have to propagate before they shock the disk gas and open a gap. We compare our relations for the gap depth and width with the previous results, and discuss their applicability to observations.

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Section: Discussionmentioning

confidence: 99%

Properties of Density and Velocity Gaps Induced by a Planet in a Protoplanetary Disk

Yun

Kim

Bae

et al. 2019

ApJ

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“…The fast inward migration of the planet causes the gaps/rings move closer to the central region after a longer evolution time. A smaller gap depth is also attributed to the high viscosity (Fung et al 2014;Kanagawa et al 2015;Zhu 2019). A shallower gap of the gas distribution for the high viscosity model leads to the dust gap and ring being shallow as well, which further makes the detection of such gap/rings harder.…”

Section: Disk Viscositymentioning

confidence: 96%

On the Dust Signatures Induced by Eccentric Super-Earths in Protoplanetary Disks

et al. 2019

ApJ

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We investigate the impact of a highly eccentric 10 M ⊕ (where M ⊕ is the Earth mass) planet embedded in a dusty protoplanetary disk on the dust dynamics and its observational implications. By carrying out high-resolution 2D gas and dust two-fluid hydrodynamical simulations, we find that the planet's orbit can be circularized at large radii. After the planet's orbit is circularized, partial gap opening and dust ring formation happen close to the planet's circularization radius, which can explain the observed gaps/rings at the outer region of disks. When the disk mass and viscosity become low, we find that an eccentric planet can even open gaps and produce dust rings close to the pericenter and apocenter radii before its circularization. This offers alternative scenarios for explaining the observed dust rings and gaps in protoplanetary disks. A lower disk viscosity is favored to produce brighter rings in observations. An eccentric planet can also potentially slow down the dust radial drift in the outer region of the disk when the disk viscosity is low (α 2 × 10 −4 ) and the circularization is faster than the dust radial drift.

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“…In that case, the inner disk can break from the outer disk and precess independently from the outer disk (e.g., Bitsch et al 2013;Xiang-Gruess & Papaloizou 2013;Nealon et al 2018). Zhu (2019) studied the effect of an inclined planet, held on a fixed orbit, on the depth and width of the gap and show that the breaking happens under the condition that the gap carved by the planet is deep enough or that the disk viscosity is very low. Alternatively, secular precession resonances can lead to large misalignments between the inner and outer disks if the companion is quite massive and no viscosity is considered (0.1-0.01 M , Owen & Lai 2017).…”

Section: Origin Of the Misalignmentsmentioning

confidence: 99%

Shadowing and multiple rings in the protoplanetary disk of HD 139614

Muro-Arena

Benisty

Ginski

et al. 2020

A&A

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Context. Shadows in scattered light images of protoplanetary disks are a common feature and support the presence of warps or misalignments between disk regions. These warps are possibly due to an inclined (sub-)stellar companion embedded in the disk. Aims. We study the morphology of the protoplanetary disk around the Herbig Ae star HD 139614 based on the first scattered light observations of this disk, which we model with the radiative transfer code MCMax3D. Methods. We obtained J-and H-band observations in polarized scattered light with VLT/SPHERE that show strong azimuthal asymmetries. In the outer disk, beyond ∼30 au, a broad shadow spans a range of ∼240 deg in position angle, in the East. A bright ring at ∼16 au also shows an azimuthally asymmetric brightness, with the faintest side roughly coincidental with the brightest region of the outer disk. Additionally, two arcs are detected at ∼34 au and ∼50 au. We created a simple 4-zone approximation to a warped disk model of HD 139614 in order to qualitatively reproduce these features. The location and misalignment of the disk components were constrained from the shape and location of the shadows they cast. Results. We find that the shadow on the outer disk covers a range of position angle too wide to be explained by a single inner misaligned component. Our model requires a minimum of two separate misaligned zones -or a continuously warped region -to cast this broad shadow on the outer disk. A small misalignment of ∼4 • between adjacent components can reproduce most of the observed shadow features. Conclusions. Multiple misaligned disk zones, potentially mimicing a warp, can explain the observed broad shadows in the HD 139614 disk. A planetary mass companion in the disk, located on an inclined orbit, could be responsible for such a feature and for the dust depleted gap responsible for a dip in the SED.

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Inclined massive planets in a protoplanetary disc: gap opening, disc breaking, and observational signatures

Cited by 88 publications

References 107 publications

Properties of Density and Velocity Gaps Induced by a Planet in a Protoplanetary Disk

Properties of Density and Velocity Gaps Induced by a Planet in a Protoplanetary Disk

On the Dust Signatures Induced by Eccentric Super-Earths in Protoplanetary Disks

Shadowing and multiple rings in the protoplanetary disk of HD 139614

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