How Empty Are Disk Gaps Opened by Giant Planets?

Fung, Jeffrey; Shi, Ji-Ming; Chiang, Eugene

doi:10.1088/0004-637x/782/2/88

Cited by 265 publications

(341 citation statements)

References 38 publications

(64 reference statements)

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“…Because our interest is focussed on the influence of the gas surface density carved by planets on the radial dust evolution, we use an approximation of the radial shape of the gaps in protoplanetary disks rather than full hydrodynamical simulations. We assume the analytical results presented in Crida et al (2006) and Fung et al (2014). Crida et al (2006) proposed an equilibrium profile considering the viscous torque (t ν ), gravitational torque (t g ), and the torque removed by pressure supported waves or pressure torque (t P ).…”

Section: Carved Gapsmentioning

confidence: 99%

“…An analytical solution for the depth of the gap close to the planet is difficult to calculate because of the strong tidal gravitational field of the planet in this region. Using two independent codes (PEnGUIn and ZEUS90), Fung et al (2014) provided an empirical relation of the depth of the gap carved by a nonmigrating giant planet in a locally isothermal disk. They consider a large parameter space for the planet-stellar mass ratio q, viscosity α, and aspect ratio H/r, finding very similar results with both codes.…”

Section: Carved Gapsmentioning

confidence: 99%

“…Additional azimuthal features that may exist when a massive planet interacts with the disk, such as vortices or spiral arms (e.g. Kley & Dirksen 2006;Ataiee et al 2013;Fung et al 2014;Zhu & Stone 2014;Juhasz et al 2015), are not considered in this work. Instead, we focus on the radial distribution of particles.…”

Section: Carved Gapsmentioning

confidence: 99%

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Sequential planet formation in the HD 100546 protoplanetary disk?

Pinilla

Birnstiel

Walsh

2015

A&A

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Context. The disk around the Herbig Ae star, HD 100546, shows structures that suggest the presence of two companions in the disk at ∼10 and ∼70 AU. The outer companion seems to be in the act of formation. Aims. Our aims are to provide constraints on the age of the planets in HD 100546 and to explore the potential evidence for sequential planet formation in transition disks such as HD 100546. Methods. We compare the recent resolved continuum observations of the disk around HD 100546 with the results of dust evolution simulations using an analytical prescription for the shapes of gaps carved by massive planets.Results. An inner pressure bump must have been present since early in the disk lifetime to have good agreement between the dust evolution models and the continuum observations of HD 100546. This pressure bump may have resulted from the presence of a very massive planet (∼20 M Jup ), which formed early in the inner disk (r ∼ 10 AU). If only this single planet exists, the disk is likely to be old, comparable to the stellar age (∼5−10 Myr). Another possible explanation is an additional massive planet in the outer disk (r ∼ 70 AU): either a low-mass outer planet ( < ∼ 5 M Jup ) injected at early times, or a higher mass outer planet ( > ∼ 15 M Jup ) formed very recently, traps the right amount of dust in pressure bumps to reproduce the observations. In the latter case, the disk could be much younger (∼3.0 Myr). Conclusions. In the case in which two massive companions are embedded in the disk around HD 100546, as suggested in the literature, the outer companion could be at least > ∼ 2.5 Myr younger than the inner companion.

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Section: Carved Gapsmentioning

confidence: 99%

Section: Carved Gapsmentioning

confidence: 99%

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Sequential planet formation in the HD 100546 protoplanetary disk?

Pinilla

Birnstiel

Walsh

2015

A&A

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“…This results in a dust ring of millimeter-sized dust, or radial dust trap (Pinilla et al 2012). The decrease in gas density due to companion clearing depends on the mass of the companion and other parameters such as the viscosity (Zhu et al 2011;Dodson-Robinson & Salyk 2011;Pinilla et al 2012;Mulders et al 2013;Fung et al 2014). Other effects that play a role in dynamic clearing are for example migration and planet accretion luminosity (e.g., Kley & Nelson 2012).…”

Section: Introductionmentioning

confidence: 99%

Gas density drops inside dust cavities of transitional disks around young stars observed with ALMA

Marel

Dishoeck

Bruderer

et al. 2015

A&A

160

215

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Context. Transitional disks with large dust cavities are important laboratories in which to study planet formation and disk evolution. Cold gas may still be present inside these cavities, but quantying this gas is challenging. The gas content is important for constraining the origin of the dust cavity. Aims. We use Atacama Large Millimeter/submillimeter Array (ALMA) observations of 12 CO 6-5 and 690 GHz (Band 9) continuum of five well-studied transitional disks. In addition, we analyze previously published Band 7 observations of a disk in the 12 CO 3-2 line and 345 GHz continuum. The observations are used to set constraints on the gas and dust surface density profiles, in particular, the drop δ gas of the gas density inside the dust cavity. Methods. The physical-chemical modeling code DALI was used to simultaneously analyze the gas and dust images. We modeled SR21, HD 135344B, LkCa15, SR24S, and RX J1615-3255 (Band 9) and J1604-2130 (Band 7). The spectral energy distribution and continuum visibility curve constrain the dust surface density. Then we used the same model to calculate the 12 CO emission, which we compared with the observations through spectra and intensity cuts. The amount of gas inside the cavity was quantified by varying the δ gas parameter. Results. Model fits to the dust and gas indicate that gas is still present inside the dust cavity for all disks, but at a reduced level. The gas surface density drops inside the cavity by at least a factor 10, while the dust density drops by at least a factor 1000. Disk masses are comparable with previous estimates from the literature, cavity radii are found to be smaller than in the data obtained with the 345 GHz SubMillimeter Array. Conclusions. The derived gas surface density profiles suggest that the cavity was cleared by one or more companions in all cases, which trapped the millimeter-sized dust at the edge of the cavity.

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“…The depth and shape of the gap depend primarily on the planet mass and the disk viscosity (Zhu et al 2011;Pinilla et al 2012;Fung et al 2014). These models show that a planet does not create a steep gas gap, but a gradual decrease over several AUs.…”

Section: Introductionmentioning

confidence: 99%

Resolved gas cavities in transitional disks inferred from CO isotopologs with ALMA

Marel

Dishoeck

Bruderer

et al. 2015

A&A

195

197

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Context. Transitional disks around young stars with large dust cavities are promising candidates to look for recently formed, embedded planets. Models of planet-disk interaction predict that young planets clear a gap in the gas while trapping dust at larger radii. Other physical mechanisms might also be responsible for cavities. Previous observations have revealed that gas is still present inside these cavities, but the spatial distribution of this gas remains uncertain. Aims. We present high spatial resolution observations with the Atacama Large Millimeter/submillimeter Array (ALMA) of 13 CO and C 18 O 3−2 or 6−5 lines of four well-studied transitional disks around pre-main-sequence stars with large dust cavities. The line and continuum observations are used to set constraints on the the gas surface density, specifically on the cavity size and density drop inside the cavity. Methods. The physical-chemical model DALI was used to analyze the gas images of SR21, HD 135344B (also known as SAO 206462), DoAr44, and IRS 48. The main parameters of interest are the size, depth and shape of the gas cavity in each of the disks. CO isotope-selective photodissociation is included to properly constrain the surface density in the outer disk from C 18 O emission. Results. The gas cavities are up to three times smaller than those of the dust in all four disks. Model fits indicate that the surface density inside the gas cavities decreases by a factor of 100 to 10 000 compared with the surface density profile derived from the outer disk. The data can be fit by either introducing one or two drops in the gas surface density or a surface density profile that increases with radius inside the cavity. A comparison with an analytical model of gap depths by planet-disk interaction shows that the disk viscosities are most likely low, between between 10 −3 and 10 −4 , for reasonable estimates of planet masses of up to 10 Jupiter masses. Conclusions. The resolved measurements of the gas and dust in transition disk cavities support the predictions of models that describe how planet-disk interactions sculpt gas disk structures and influence the evolution of dust grains. These observed structures strongly suggest the presence of giant planetary companions in transition disk cavities, although at smaller orbital radii than is typically indicated from the dust cavity radii alone.

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How Empty Are Disk Gaps Opened by Giant Planets?

Cited by 265 publications

References 38 publications

Sequential planet formation in the HD 100546 protoplanetary disk?

Sequential planet formation in the HD 100546 protoplanetary disk?

Gas density drops inside dust cavities of transitional disks around young stars observed with ALMA

Resolved gas cavities in transitional disks inferred from CO isotopologs with ALMA

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