Gas Flow across Gaps in Protoplanetary Disks

Lubow, S. H.; D’Angelo, Gennaro

doi:10.1086/500356

Cited by 256 publications

(315 citation statements)

References 28 publications

Supporting

Mentioning

292

Contrasting

Order By: Relevance

“…A single planet of a few M Jup carves only a narrow gap (typically Δr gap /r gap ∼ 0.1) about its orbit in a viscous disk that is a few times more massive than the planet and as soon as the Hill's radius 5 is larger than the disk height (e.g., Lubow & D'Angelo 2006). This is not compatible with the large inner hole/gap observed in most transitional disks.…”

Section: Planetary Companionsmentioning

confidence: 93%

Ruling out unresolved binaries in five transitional disks

Vicente

Merın

Hartung

et al. 2011

A&A

View full text Add to dashboard Cite

Context. The presence of unresolved binaries on sub-arsecond scales could explain the existence of optically thin inner holes or gaps in circumstellar disks, which are commonly referred to as "transitional" or "cold" disks, and it is the first scenario to check before making any other assumptions. Aims. We aim at detecting the presence of companions inside the inner hole/gap region of a sample of five well known transitional disks using spatially-resolved imaging in the near-IR with the VLT/NACO/S13 camera, which probes projected distances from the primary of typically 0.1 to 7 arcsec. The sample includes the stars DoAr 21, HD 135344B (SAO 206462), HR 4796A, T Cha, and TW Hya, spanning ages of less than 1 to 10 Myr, spectral types of A0 to K7, and hole/gap outer radii of 4 to 100 AU. Methods. In order to enhance the contrast and to avoid saturation at the core of the point-spread function (PSF), we use narrow-band filters at 1.75 and 2.12 μm. The "locally optimized combination of images" (LOCI) algorithm is applied for an optimal speckle noise removal and PSF subtraction, providing an increase of 0.5-1.5 mag in contrast over the classic method. Results. With the proviso that we could have missed companions owing to unfavorable projections, the VLT/NACO observations rule out the presence of unresolved companions down to an inner radius of about 0. 1 from the primary in all five transitional disks and with a detection limit of 2 to 5 mag in contrast. In the disk outer regions the detection limits typically reach 8 to 9 mag in contrast and 4.7 mag for T Cha. Hence, the NACO images resolve part of the inner hole/gap region of all disks with the exception of TW Hya, for which the inner hole is only 4 AU. The 5σ sensitivity profiles, together with a selected evolutionary model, allow to discard stellar companions within the inner hole/gap region of T Cha, and down to the substellar regime for HD 135344B and HR 4796A. DoAr 21 is the only object from the sample of five disks for which the NACO images are sensitive enough for a detection of objects less massive than ∼13 M Jup that is, potential giant planets or low-mass brown dwarfs at radii larger than ∼76 AU (0. 63). Conclusions. These new VLT/NACO observations further constrain the origin of the inner opacity cavities to be owing to closer or lower-mass companions or other mechanisms such as giant planet formation, efficient grain growth, and photoevaporation (for DoAr 21 and HR 4796A).

show abstract

Section: Planetary Companionsmentioning

confidence: 93%

Ruling out unresolved binaries in five transitional disks

Vicente

Merın

Hartung

et al. 2011

A&A

View full text Add to dashboard Cite

show abstract

“…This rapid gas accretion slows down when the giant planet opens a gap in the gas disk. According to hydrodynamic simulations (Kley 1999) the planet is not entirely isolated from the ambient gas, and accretion continues along tidally generated spiral arms (Lubow & D'Angelo 2006). Therefore, gas accretion onto the planet's surface stops only when the surrounding gas is dispersed and formation of a giant planet ends with the photoevaporation of the gas disk.…”

Section: Disk Dispersal In the Classic Core Accretion Scenariomentioning

confidence: 99%

Disk Dispersal: Theoretical Understanding and Observational Constraints

et al. 2016

View full text Add to dashboard Cite

Protoplanetary disks dissipate rapidly after the central star forms, on time-scales comparable to those inferred for planet formation. In order to allow the formation of planets, disks must survive the dispersive effects of UV and X-ray photoevaporation for at least a few Myr. Viscous accretion depletes significant amounts of the mass in gas and solids, while photoevaporative flows driven by internal and external irradiation remove most of the gas. A reasonably large fraction of the mass in solids and some gas get incorporated into planets. Here, we review our current understanding of disk evolution and dispersal, and discuss how these might affect planet formation. We also discuss existing observational constraints on dispersal mechanisms and future directions.

show abstract

“…This function is essentially a Gaussian similar to the vertical scale height, but with a different exponent of 3 as in Lubow & D'Angelo (2006), Eq. (5).…”

Section: Rounded-off Wallmentioning

confidence: 99%

“…However, gas flows back into the gap due to pressure gradients and viscous spreading, which tends to close the gap. Therefore, the shape of the surface density around a planet depends on its mass, the disk viscosity and scale height (Crida et al 2006;Lubow & D'Angelo 2006). In general, a heavier planet can carve out a deeper and wider gap, while a more viscous or thicker disk (higher pressure scale height) will reduce the gap width and depth.…”

Section: Gap Openingmentioning

confidence: 99%

“…These rounded-off walls are a natural outcome of hydrodynamical models of disk-planet interaction, where the detailed shape of the radial surface density profile depends on planet mass, disk thickness, and viscosity (Crida et al 2006;Lubow & D'Angelo 2006). The mass of the planet will therefore be reflected in the shape of the disk wall, which can be constrained with MIDI, the mid-infrared interferometer on the Very Large Telescope.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Planet or brown dwarf? Inferring the companion mass in HD 100546 from the wall shape using mid-infrared interferometry

Mulders

Paardekooper

Panić

et al. 2013

A&A

View full text Add to dashboard Cite

Context. Giant planets form in protoplanetary disks while these disks are still gas-rich, and can reveal their presence through the annular gaps they carve out. HD 100546 is a gas-rich disk with a wide gap between a radius of ∼1 and 13 AU, possibly cleared out by a planetary companion or planetary system. Aims. We aim to identify the nature of the unseen companion near the far end of the disk gap. Methods. We used mid-infrared interferometry at multiple baselines to constrain the curvature of the disk wall at the far end of the gap. We used 2D hydrodynamical simulations of embedded planets and brown dwarfs to estimate the viscosity of the disk and the mass of a companion close to the disk wall. Results. We find that the disk wall at the far end of the gap is not vertical, but rounded-off by a gradient in the surface density. This gradient can be reproduced in hydrodynamical simulations with a single, heavy companion ( 30 . . . 80 M Jup ) while the disk has a viscosity of at least α 5 × 10 −3 . Taking into account the changes in the temperature structure after gap opening reduces the lower limit on the planet mass and disk viscosity to 20 M Jup and α = 2 × 10 −3 . Conclusions. The object in the disk gap of HD 100546 that shapes the disk wall is most likely a 60 +20 −40 M Jup brown dwarf, while the disk viscosity is estimated to be at least α = 2 × 10 −3 . The disk viscosity is an important factor in estimating planetary masses from disk morphologies: more viscous disks need heavier planets to open an equally deep gap.

show abstract

Gas Flow across Gaps in Protoplanetary Disks

Cited by 256 publications

References 28 publications

Ruling out unresolved binaries in five transitional disks

Ruling out unresolved binaries in five transitional disks

Disk Dispersal: Theoretical Understanding and Observational Constraints

Planet or brown dwarf? Inferring the companion mass in HD 100546 from the wall shape using mid-infrared interferometry

Contact Info

Product

Resources

About