ALMA OBSERVATIONS OF HD 141569’s CIRCUMSTELLAR DISK

White, Jacob Aaron; Boley, Aaron C.; Hughes, A. Meredith; Flaherty, Kevin; Wilner, David J.; Corder, Stuartt; Payne, Matthew J.

doi:10.3847/0004-637x/829/1/6

Cited by 41 publications

(94 citation statements)

References 58 publications

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“…The companion to HD142527, which is located well within the gap in the disk, is commonly interpreted as having too low a mass (0.13 M e ; Lacour et al 2016) and eccentricity to generate the observed spiral arms, so this object is included in our sample (although see Price et al 2018). Lastly, we removed HD141569 from the sample, because its low dust mass (on the order of 1 M ⊕ or less; Flaherty et al 2016;White et al 2016) makes the system prone to radiation pressure and photoelectric instability, which can also produce spiral arm structures (e.g., Richert et al 2018b). …”

Section: Disk Imaging Samplementioning

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: Disk Imaging Samplementioning

confidence: 99%

Spiral Arms in Disks: Planets or Gravitational Instability?

Dong

Najita

Brittain

2018

ApJ

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“…Millimeterwavelength interferometry provided the first spatially resolved observations of the molecular gas emission in a debris disk (Hughes et al 2008a), and the improved sensitivity and angular resolution of the Atacama Large Millimeter/submillimeter Array (ALMA) has led to a resurgence of interest in these objects, resulting in spectacular gas and dust imaging of the recently discovered HD 21997 disk Moór et al 2013), the iconic β Pictoris disk (Dent et al 2014), and recently the first gas-bearing debris disk around a solar-type star (HD 181327; Marino et al 2016). Another object of interest has been the optically thin dust disk around the 5 Myr old Herbig Ae star HD 141569, whose classification as a transitional or debris disk has been an object of intense discussion in the literature: recent observations with the Submillimeter Array (SMA) and Combined Array for Research in Millimeter-wave Astronomy (CARMA) have spatially resolved the gas disk for the first time (Flaherty et al 2016), and ALMA observations probe the disk in greater detail (White et al 2016). A survey for gas emission in a sample of 24 debris disks in the 10 Myr old Sco-Cen star-forming region has revealed that gas-rich debris disks are common around intermediate-mass stars, with gas detected around three of the seven A/B stars in the sample, but rare around FGK stars (Lieman-Sifry et al 2016).…”

Section: Introductionmentioning

confidence: 99%

Radial Surface Density Profiles of Gas and Dust in the Debris Disk around 49 Ceti

Hughes

Lieman-Sifry

Flaherty

et al. 2017

ApJ

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127

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We present ∼0 4 resolution images of CO(3-2) and associated continuum emission from the gas-bearing debris disk around the nearby A star 49 Ceti, observed with the Atacama Large Millimeter/Submillimeter Array (ALMA). We analyze the ALMA visibilities in tandem with the broadband spectral energy distribution to measure the radial surface density profiles of dust and gas emission from the system. The dust surface density decreases with radius between ∼100 and 310 au, with a marginally significant enhancement of surface density at a radius of ∼110 au. The SED requires an inner disk of small grains in addition to the outer disk of larger grains resolved by ALMA. The gas disk exhibits a surface density profile that increases with radius, contrary to most previous spatially resolved observations of circumstellar gas disks. While ∼80% of the CO flux is well described by an axisymmetric power-law disk in Keplerian rotation about the central star, residuals at ∼20% of the peak flux exhibit a departure from axisymmetry suggestive of spiral arms or a warp in the gas disk. The radial extent of the gas disk (∼220 au) is smaller than that of the dust disk (∼300 au), consistent with recent observations of other gasbearing debris disks. While there are so far only three broad debris disks with wellcharacterized radial dust profiles at millimeter wavelengths, 49 Ceti's disk shows a markedly different structure from two radially resolved gas-poor debris disks, implying that the physical processes generating and sculpting the gas and dust are fundamentally different.

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“…[O I] and [C II] emissions were also detected for β Pictoris (Brandeker et al 2016). Some debris disks are known to have submillimeter-wave CO emission; e.g., 49 Ceti (Dent et al 2005;Hughes et al 2008), β Pictoris (Fernández et al 2006;Dent et al 2014), HD 21997 (Moór et al 2011Kóspál et al 2013), HD 131835 (Moór et al 2015), and HD 141569 (White et al 2016).…”

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confidence: 99%

Detection of Submillimeter-wave [C i] Emission in Gaseous Debris Disks of 49 Ceti and β Pictoris

Higuchi

Sato

Tsukagoshi

et al. 2017

ApJL

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We have detected [C I]3 P 1 -3 P 0 emissions in the gaseous debris disks of 49 Ceti and β Pictoris with the 10 m telescope of the Atacama Submillimeter Telescope Experiment, which is the first detection of such emissions. The line profiles of [C I] are found to resemble those of CO(J=3-2) observed with the same telescope and the Atacama Large Millimeter/submillimeter Array. This result suggests that atomic carbon (C) coexists with CO in the debris disks, and is likely formed by the photodissociation of CO. Assuming an optically thin [C I] emission with the excitation temperature ranging from 30 to 100 K, the column density of C is evaluated to be (2.2±0.2)×10 17 and (2.5±0.7)×10 16 cm −2 for 49 Ceti and β Pictoris, respectively. The C/CO column density ratio is thus derived to be 54±19 and 69±42 for 49 Ceti and β Pictoris, respectively. These ratios are higher than those of molecular clouds and diffuse clouds by an order of magnitude. The unusually high ratios of C to CO are likely attributed to a lack of H 2 molecules needed to reproduce CO molecules efficiently from C. This result implies a small number of H 2 molecules in the gas disk; i.e., there is an appreciable contribution of secondary gas from dust grains.

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ALMA OBSERVATIONS OF HD 141569’s CIRCUMSTELLAR DISK

Cited by 41 publications

References 58 publications

Spiral Arms in Disks: Planets or Gravitational Instability?

Spiral Arms in Disks: Planets or Gravitational Instability?

Radial Surface Density Profiles of Gas and Dust in the Debris Disk around 49 Ceti

Detection of Submillimeter-wave [C i] Emission in Gaseous Debris Disks of 49 Ceti and β Pictoris

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