Protoplanetary Disks in ρ Ophiuchus as Seen from ALMA

Cox, Erin G.; Harris, Robert J.; Looney, Leslie W.; Chiang, Hsin Fang; Chandler, Claire J.; Kratter, Kaitlin M.; Li, Zhi Yun; Pérez, Laura; Tobin, John J.

doi:10.3847/1538-4357/aa97e2

Cited by 106 publications

(161 citation statements)

References 88 publications

(118 reference statements)

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“…These observed disks surrounding a range of host-stellar masses have gas radii in the range of 63-500 AU at an age of ∼ 1-3 Myr. We emphasize, however, that these large, extended disks are the exception and are not indicative of typical disks that are much more compact, as indicated by numerous observations showing dust radii of 20 − 30 AU (Barenfeld et al 2016(Barenfeld et al , 2017Cox et al 2017;Hendler et al 2017;Tazzari et al 2017;Cieza et al 2019;Long et al 2019).…”

Section: Introductionmentioning

confidence: 67%

Formation of planetary populations − II. Effects of initial disc size and radial dust drift

Alessi

Cridland

2020

Monthly Notices of the Royal Astronomical Society

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Recent ALMA observations indicate that while a range of disk sizes exist, typical disk radii are small, and that radial dust drift affects the distribution of solids in disks.Here we explore the consequences of these features in planet population synthesis models. A key feature of our model is planet traps -barriers to otherwise rapid type-I migration of forming planets -for which we include the ice line, heat transition, and outer edge of the dead zone. We find that the ice line plays a fundamental role in the formation of warm Jupiters. In particular, the ratio of super Earths to warm Jupiters formed at the ice line depend sensitively on the initial disk radius. Initial gas disk radii of ∼50 AU results in the largest super Earth populations, while both larger and smaller disk sizes result in the ice line producing more gas giants near 1 AU. This transition between typical planet class formed at the ice line at various disk radii confirms that planet formation is fundamentally linked to disk properties (in this case, disk size), and is a result that is only seen when dust evolution effects are included in our models. Additionally, we find that including radial dust drift results in the formation of more super Earths between 0.1 -1 AU, having shorter orbital radii than those produced in models where dust evolution effects are not included.

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Section: Introductionmentioning

confidence: 67%

Formation of planetary populations − II. Effects of initial disc size and radial dust drift

Alessi

Cridland

2020

Monthly Notices of the Royal Astronomical Society

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“…van der Marel et al (2015) hinted at the presence of a dust gap in the outer part of the disk between 110 and 130 au from the ALMA resulting image of the same data set. The disk around ρOph38 has a two-ringed-like structure as described in Cox et al (2017). For the analysis and discussion in the following sections, we do not consider these three disks because we only keep TDs with a cavity and a single ring of emission.…”

Section: Data Analysis and Resultsmentioning

confidence: 99%

“…Perez). Finally, we include two newly discovered TDs in the ρ Ophiuchus molecular cloud: ρOph 3 and ρOph 38 (Cox et al 2017). Several disks of this sample have been reobserved in more recent years with higher resolution and sensitivity (e.g., HD 100546); however, we prefer to use the data that have already been published to create a homogeneous sample at medium resolution.…”

Section: Observations and Sample Of Tdsmentioning

confidence: 99%

Homogeneous Analysis of the Dust Morphology of Transition Disks Observed with ALMA: Investigating Dust Trapping and the Origin of the Cavities

Pinilla

Tazzari

Pascucci

et al. 2018

ApJ

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103

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We analyze the dust morphology of 29 transition disks (TDs) observed with Atacama Large (sub-)Millimeter Array (ALMA) at (sub-)millimeter emission. We perform the analysis in the visibility plane to characterize the total flux, cavity size, and shape of the ring-like structure. First, we found that the M dust -M å relation is much flatter for TDs than the observed trends from samples of class II sources in different star-forming regions. This relation demonstrates that cavities open in high (dust) mass disks, independent of the stellar mass. The flatness of this relation contradicts the idea that TDs are a more evolved set of disks. Two potential reasons (not mutually exclusive) may explain this flat relation: the emission is optically thick or/and millimeter-sized particles are trapped in a pressure bump. Second, we discuss our results of the cavity size and ring width in the context of different physical processes for cavity formation. Photoevaporation is an unlikely leading mechanism for the origin of the cavity of any of the targets in the sample. Embedded giant planets or dead zones remain as potential explanations. Although both models predict correlations between the cavity size and the ring shape for different stellar and disk properties, we demonstrate that with the current resolution of the observations, it is difficult to obtain these correlations. Future observations with higher angular resolution observations of TDs with ALMA will help discern between different potential origins of cavities in TDs.

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“…Some transition disks have been discovered serendipitously as part of complete disk surveys of nearby star forming regions (e.g. Ansdell et al 2016b;Pascucci et al 2016;Cox et al 2017;Long et al 2018) at lower spatial resolution (∼0.12-0.3"). However, for many disks identified in those surveys the resolution was insufficient to fully resolve the cavity and they were thus not included.…”

Section: Sample Selectionmentioning

confidence: 99%

Dust-depleted Inner Disks in a Large Sample of Transition Disks through Long-baseline ALMA Observations

Francis

Marel

2020

ApJ

160

146

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Transition disks with large inner dust cavities are thought to host massive companions. However, the disk structure inside the companion orbit and how material flows toward an actively accreting star remain unclear. We present a high resolution continuum study of inner disks in the cavities of 38 transition disks. Measurements of the dust mass from archival Atacama Large Millimeter/Submillimeter Array observations are combined with stellar properties and spectral energy distributions to assemble a detailed picture of the inner disk. An inner dust disk is detected in 18 of 38 disks in our sample. Of the 14 resolved disks, 8 are significantly misaligned with the outer disk. The near-infrared excess is uncorrelated with the mm dust mass of the inner disk. The size-luminosity correlation known for protoplanetary disks is recovered for the inner disks as well, consistent with radial drift. The inner disks are depleted in dust relative to the outer disk and their dust mass is uncorrelated with the accretion rates. This is interpreted as the result of radial drift and trapping by planets in a low α (∼ 10 −3 ) disk, or a failure of the α-disk model to describe angular momentum transport and accretion. The only disk in our sample with confirmed planets in the gap, PDS 70, has an inner disk with a significantly larger radius and lower inferred gas-to-dust ratio than other disks in the sample. We hypothesize that these inner disk properties and the detection of planets are due to the gap having only been opened recently by young, actively accreting planets.

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Protoplanetary Disks in ρ Ophiuchus as Seen from ALMA

Cited by 106 publications

References 88 publications

Formation of planetary populations − II. Effects of initial disc size and radial dust drift

Formation of planetary populations − II. Effects of initial disc size and radial dust drift

Homogeneous Analysis of the Dust Morphology of Transition Disks Observed with ALMA: Investigating Dust Trapping and the Origin of the Cavities

Dust-depleted Inner Disks in a Large Sample of Transition Disks through Long-baseline ALMA Observations

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