Lopsided dust rings in transition disks

Birnstiel, T.; Dullemond, C. P.; Pinilla, P.

doi:10.1051/0004-6361/201220847

Cited by 157 publications

(185 citation statements)

References 43 publications

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“…This cannot be confirmed because of the unknown vertical mixing of the gas and dust. Finally, a nondetection of an overdensity in the gas is consistent with the dust-trapping scenario: a vortex in the gas may already have disappeared while the created dust asymmetry remains because the time scale of smoothing out a dust asymmetry is on the order of several Myr (Birnstiel et al 2013).…”

Section: Origin Of the H 2 Co Emissionsupporting

confidence: 62%

Warm formaldehyde in the Ophiuchus IRS 48 transitional disk

Marel

Dishoeck

Bruderer

et al. 2014

A&A

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Context. Simple molecules such as H 2 CO and CH 3 OH in protoplanetary disks are the starting point for the production of more complex organic molecules. So far, the observed chemical complexity in disks has been limited because of freeze-out of molecules onto grains in the bulk of the cold outer disk. Aims. Complex molecules can be studied more directly in transitional disks with large inner holes because these have a higher potential of detection through the UV heating of the outer disk and the directly exposed midplane at the wall. Methods. We used Atacama Large Millimeter/submillimeter Array (ALMA) Band 9 (∼680 GHz) line data of the transitional disk Oph IRS 48, which was previously shown to have a large dust trap, to search for complex molecules in regions where planetesimals are forming. Results. We report the detection of the H 2 CO 9(1, 8)-8(1, 7) line at 674 GHz, which is spatially resolved as a semi-ring at ∼60 AU radius centered south from the star. The inferred H 2 CO abundance is ∼10 −8 , derived by combining a physical disk model of the source with a non-LTE excitation calculation. Upper limits for CH 3 OH lines in the same disk give an abundance ratio H 2 CO/CH 3 OH >0.3, which indicates that both ice formation and gas-phase routes play a role in the H 2 CO production. Upper limits on the abundances of H 13 CO + , CN and several other molecules in the disk were also derived and found to be consistent with full chemical models.Conclusions. The detection of the H 2 CO line demonstrates the start of complex organic molecules in a planet-forming disk. Future ALMA observations are expected to reduce the abundance detection limits of other molecules by 1−2 orders of magnitude and test chemical models of organic molecules in (transitional) disks.

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Section: Origin Of the H 2 Co Emissionsupporting

confidence: 62%

Warm formaldehyde in the Ophiuchus IRS 48 transitional disk

Marel

Dishoeck

Bruderer

et al. 2014

A&A

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“…At the position of the continuum peak, CO emission is detected, but not particularly strong. This is however not inconsistent with a pressure maximum at this position, because 12 CO is likely optically thick and a weak increase in density by less than a factor of 2 is sufficient to trigger dust trapping (Birnstiel et al 2013; see further discussion in Sect. 5.2).…”

Section: Observations and Data Reductionmentioning

confidence: 81%

“…The planet/companion-disk interaction can also induce perturbations in the gas structure leading to local gas pressure maxima. These pressure maxima can prevent large ( mm-sized) dust grains from quickly drifting towards the star before planet formation through dust coagulation and core accretion can take place (e.g., Whipple 1972;Rice et al 2006;Alexander & Armitage 2007;Garaud 2007;Kretke & Lin 2007;Dzyurkevich et al 2010;Pinilla et al 2012;Birnstiel et al 2013;Lyra & Lin 2013). Thus, the gas structure in transition disks is of direct importance for planet formation.…”

Section: Introductionmentioning

confidence: 99%

Gas structure inside dust cavities of transition disks: Ophiuchus IRS 48 observed by ALMA

Bruderer

Marel

Dishoeck

et al. 2014

A&A

134

196

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Context. Transition disks are recognized by the absence of emission of small dust grains inside a radius of up to several 10s of AUs. Owing to the lack of angular resolution and sensitivity, the gas content of these dust holes has not yet been determined, but is of importance for constraining the mechanism leading to the dust holes. It is thought that transition disks are currently undergoing the process of dispersal, setting an end to the giant planet formation process. Aims. We present new high-resolution observations with the Atacama Large Millimeter/submillimeter Array (ALMA) of gas lines towards the transition disk Oph IRS 48 previously shown to host a large dust trap. The ALMA telescope has detected the J = 6−5 line of 12 CO and C 17 O around 690 GHz (434 μm) at a resolution of ∼0.25 corresponding to ∼30 AU (FWHM). The observed gas lines are used to set constraints on the gas surface density profile. Methods. New models of the physical-chemical structure of gas and dust in Oph IRS 48 are developed to reproduce the CO line emission together with the spectral energy distribution and the VLT-VISIR 18.7 μm dust continuum images. Integrated intensity cuts and the total spectrum from models having different trial gas surface density profiles are compared to observations. The main parameters varied are the drop in gas surface density inside the dust-free cavity with a radius of 60 AU and inside the gas-depleted innermost 20 AU. Using the derived surface density profiles, predictions for other CO isotopologues are made, which can be tested by future ALMA observations of the object. Results. From the ALMA data we find a total gas mass of the disk of 1.4 × 10 −4 M . This gas mass yields a gas-to-dust ratio of ∼10, but with considerable uncertainty. Inside 60 AU, the gas surface density drops by a factor of ∼12 for an assumed surface density slope of γ = 1 (Σ ∝ r −γ ). Inside 20 AU, the gas surface density drops by a factor of at least 110. The drops are measured relative to the extrapolation to small radii of the surface density law at radii >60 AU. The inner radius of the gas disk at 20 AU can be constrained to better than ±5 AU. Conclusions. The derived gas surface density profile points to the clearing of the cavity by one or more massive planets/companions rather than just photoevaporation or grain-growth.

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“…This model has been used extensively to investigate dust distributions in different types of disks, including comparisons with observations (e.g. Birnstiel et al 2013;van der Marel et al 2013;Pinilla et al 2013;de Juan Ovelar et al 2013). We investigate the evolution of 180 species of dust grains, defined by size from 1 µm to 200 cm.…”

Section: Dust Evolution and Radial Gas Velocitymentioning

confidence: 99%

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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Lopsided dust rings in transition disks

Cited by 157 publications

References 43 publications

Warm formaldehyde in the Ophiuchus IRS 48 transitional disk

Warm formaldehyde in the Ophiuchus IRS 48 transitional disk

Gas structure inside dust cavities of transition disks: Ophiuchus IRS 48 observed by ALMA

Sequential planet formation in the HD 100546 protoplanetary disk?

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