Erratum: “Observational Signatures of Planets in Protoplanetary Disks. I. Gaps Opened by Single and Multiple Young Planets in Disks” (2015, ApJ, 809, 93)

Dong, Ruobing; Zhu, Zhaohuan; Whitney, B. A.

doi:10.3847/1538-4357/aa73d5

Cited by 185 publications

(258 citation statements)

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“…More graphically, high-resolution submillimeter continuum images of disks made with ALMA commonly show stunning rings and gaps (ALMA Partnership et al 2015;Andrews et al 2016;Cieza et al 2016Cieza et al , 2017Isella et al 2016;Loomis et al 2017;Dipierro et al 2018;Fedele et al 2018;Huang et al 2018), structures that signal that disk solids have grown beyond centimeter sizes and possibly into planetary-mass objects (e.g., Dipierro et al 2015;Dong et al 2015cDong et al , 2017a). These results exclaim that disks are highly evolved and call into question disk mass estimates made under the usual assumption of simple, unevolved, optically thin disks.…”

Section: Introductionmentioning

confidence: 99%

Spiral Arms in Disks: Planets or Gravitational Instability?

Dong

Najita

Brittain

2018

ApJ

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Spiral arm structures seen in scattered-light observations of protoplanetary disks can potentially serve as signposts of planetary companions. They can also lend unique insights into disk masses, which are critical in setting the mass budget for planet formation but are difficult to determine directly. A surprisingly high fraction of disks that have been well studied in scattered light have spiral arms of some kind (8/29), as do a high fraction (6/11) of wellstudied Herbig intermediate-mass stars (i.e., Herbig stars >1.5 M e ). Here we explore the origin of spiral arms in Herbig systems by studying their occurrence rates, disk properties, and stellar accretion rates. We find that two-arm spirals are more common in disks surrounding Herbig intermediate-mass stars than are directly imaged giant planet companions to mature A and B stars. If two-arm spirals are produced by such giant planets, this discrepancy suggests that giant planets are much fainter than predicted by hot-start models. In addition, the high stellar accretion rates of Herbig stars, if sustained over a reasonable fraction of their lifetimes, suggest that disk masses are much larger than inferred from their submillimeter continuum emission. As a result, gravitational instability is a possible explanation for multiarm spirals. Future observations can lend insights into the issues raised here.

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Section: Introductionmentioning

confidence: 99%

Spiral Arms in Disks: Planets or Gravitational Instability?

Dong

Najita

Brittain

2018

ApJ

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“…The HL Tau system, which is now known to have a series of narrow gaps in its disk (e.g., ALMA Partnership et al 2015), is thought to be somewhere between the Class I and II stages and is likely ∼1 Myr old. If the gaps are carved by planets (Dong et al 2015), it would be an indication that planet formation must begin early enough to form Saturn-mass planets (e.g., Dong et al 2015;Kanagawa et al 2015) within the first ∼1 Myr. Perhaps even more interesting, several Class I protoplanetary disks have recently been found to also exhibit similar features.…”

Section: Implications For Giant Planet Formationmentioning

confidence: 99%

Disk Masses for Embedded Class I Protostars in the Taurus Molecular Cloud

Sheehan

Eisner

2017

ApJ

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Class I protostars are thought to represent an early stage in the lifetime of protoplanetary disks, when they are still embedded in their natal envelope. Here we measure the disk masses of 10 Class I protostars in the Taurus Molecular Cloud to constrain the initial mass budget for forming planets in disks. We use radiative transfer modeling to produce synthetic protostar observations and fit the models to a multi-wavelength data set using a Markov Chain Monte Carlo fitting procedure. We fit these models simultaneously to our new Combined Array for Research in Millimeter-wave Astronomy 1.3 mm observations that are sensitive to the wide range of spatial scales that are expected from protostellar disks and envelopes so as to be able to distinguish each component, as well as broadband spectral energy distributions compiled from the literature. We find a median disk mass of  M 0.018 on average, more massive than the Taurus Class II disks, which have median disk mass of~ M 0.0025 . This decrease in disk mass can be explained if dust grains have grown by a factor of 75 in grain size, indicating that by the Class II stage, at a few Myr, a significant amount of dust grain processing has occurred. However, there is evidence that significant dust processing has occurred even during the Class I stage, so it is likely that the initial mass budget is higher than the value quoted here.

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“…Once a planetary core has gained sufficient mass to undergo runaway gas accretion, it may interact strongly with the protoplanetary disk, driving large-scale disk structures, such as gaps (e.g., Jang-Condell & Turner 2012, and Dong et al 2015b, vortices (e.g., Hammer et al 2017), and spiral density waves (e.g., Dong et al 2015a;Zhu et al 2015). These interactions contribute to the disk evolution and may significantly alter the environment of planet formation.…”

Section: Introductionmentioning

confidence: 99%

The Orbit of the Companion to HD 100453A: Binary-driven Spiral Arms in a Protoplanetary Disk

Wagner

Dong

Sheehan

et al. 2018

ApJ

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HD 100453AB is a 10±2 Myr old binary whose protoplanetary disk was recently revealed to host a global twoarmed spiral structure. Given the relatively small projected separation of the binary (1 05, or ∼108 au), gravitational perturbations by the binary seemed to be a likely driving force behind the formation of the spiral arms. However, the orbit of these stars remained poorly understood, which prevented a proper treatment of the dynamical influence of the companion on the disk. We observed HD100453AB between 2015 and 2017, utilizing extreme adaptive optics systems on the Very Large Telescope and the Magellan Clay Telescope. We combined the astrometry from these observations with published data to constrain the parameters of the binary's orbit to a = 1 06±0 09, e=0.17±0.07, and i = 32°.5 ± 6°.5. We utilized publicly available ALMA 12 CO data to constrain the inclination of the disk,~ i 28 disk , which is relatively coplanar with the orbit of the companion and consistent with previous estimates from scattered light images. Finally, we input these constraints into hydrodynamic and radiative transfer simulations to model the structural evolution of the disk. We find that the spiral structure and truncation of the circumprimary disk in HD 100453 are consistent with a companion-driven origin. Furthermore, we find that the primary star's rotation, its outer disk, and the companion exhibit roughly the same direction of angular momentum, and thus the system likely formed from the same parent body of material.

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Erratum: “Observational Signatures of Planets in Protoplanetary Disks. I. Gaps Opened by Single and Multiple Young Planets in Disks” (2015, ApJ, 809, 93)

Cited by 185 publications

References 0 publications

Spiral Arms in Disks: Planets or Gravitational Instability?

Spiral Arms in Disks: Planets or Gravitational Instability?

Disk Masses for Embedded Class I Protostars in the Taurus Molecular Cloud

The Orbit of the Companion to HD 100453A: Binary-driven Spiral Arms in a Protoplanetary Disk

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