Fingerprints of giant planets in the photospheres of Herbig stars

Kama, M.; Folsom, C. P.; Pinilla, P.

doi:10.1051/0004-6361/201527094

Cited by 110 publications

(174 citation statements)

References 73 publications

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“…This is, together with the very low mass accretion rate, in line with the conclusions of Kama et al (2015), who propose that the depletion of heavy elements found in the stellar spectrum emerges as a Jupiter-like planet blocks the accretion of part of the dust and to lesser extent the gas.…”

Section: Large Grains and Free-free Emission Filling In The Disksupporting

confidence: 87%

Cavity and other radial substructures in the disk around HD 97048

Plas

Wright

Ménard

et al. 2016

A&A

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Context. Gaps, cavities and rings in circumstellar disks are signposts of disk evolution and planet-disk interactions. We follow the recent suggestion that Herbig Ae/Be disks with a flared disk harbour a cavity, and investigate the disk around HD 97048. Aims. We aim to resolve the 34± 4 au central cavity predicted by Maaskant et al. (2013) and to investigate the structure of the disk. Methods. We image the disk around HD 97048 using ALMA at 0.85 mm and 2.94 mm, and ATCA (multiple frequencies) observations. Our observations also include the 12 CO J=1-0, 12 CO J=3-2 and HCO + J=4-3 emission lines. Results. A central cavity in the disk around HD 97048 is resolved with a 40-46 au radius. Additional radial structure present in the surface brightness profile can be accounted for either by an opacity gap at 90 au or by an extra emitting ring at 150 au. The continuum emission tracing the dust in the disk is detected out to 355 au. The 12 CO J=3-2 disk is detected 2.4 times farther out. The 12 CO emission can be traced down to ≈ 10 au scales. Non-Keplerian kinematics are detected inside the cavity via the HCO + J=4-3 velocity map. The mm spectral index measured from ATCA observations suggests that grain growth has occurred in the HD 97048 disk. Finally, we resolve a highly inclined disk out to 150 au around the nearby 0.5 M binary ISO-ChaI 126. Conclusions. The data presented here reveal a cavity in the disk of HD 97048, and prominent radial structure in the surface brightness. The cavity size varies for different continuum frequencies and gas tracers. The gas inside the cavity follows non-Keplerian kinematics seen in HCO + emission. The variable cavity size along with the kinematical signature suggests the presence of a substellar companion or massive planet inside the cavity.

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Section: Large Grains and Free-free Emission Filling In The Disksupporting

confidence: 87%

Cavity and other radial substructures in the disk around HD 97048

Plas

Wright

Ménard

et al. 2016

A&A

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“…Second, early-type stars with metal-poor photospheres, in particular the λBoo stars, show an ultraviolet excess (Murphy & Paunzen 2017). Folsom et al (2012) and Kama et al (2015) found a relatively high fraction of HAeBes in their samples (up to ∼50%) showing the λBoo pattern to varying degrees. If this effect is common among the targets in our sample, it is possible that M  has been systematically overestimated.…”

Section: Appendix a Scattered-light Disk Samplementioning

confidence: 96%

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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“…The photospheric abundances of Herbig Ae/Be stars were recently shown to be a predictor of the inner disk gas and dust content (Kama et al 2015). This is in contrast to T Tauri stars, which have convective envelopes, where mixing rapidly erases accretion signatures.…”

Section: The Return Of Volatiles To the Gas In The Inner Diskmentioning

confidence: 99%

Volatile-carbon locking and release in protoplanetary disks

Kama

Bruderer

Dishoeck

et al. 2016

A&A

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201

312

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Aims. The composition of planetary solids and gases is largely rooted in the processing of volatile elements in protoplanetary disks. To shed light on the key processes, we carry out a comparative analysis of the gas-phase carbon abundance in two systems with a similar age and disk mass, but different central stars: HD 100546 and TW Hya. Methods. We combine our recent detections of C 0 in these disks with observations of other carbon reservoirs (CO, C + , C 2 H) and gas-mass and warm-gas tracers (HD, O 0 ), as well as spatially resolved ALMA observations and the spectral energy distribution. The disks are modelled with the DALI 2D physical-chemical code. Stellar abundances for HD 100546 are derived from archival spectra. Results. Upper limits on HD emission from HD 100546 place an upper limit on the total disk mass of ≤0.1 M . The gas-phase carbon abundance in the atmosphere of this warm Herbig disk is, at most, moderately depleted compared to the interstellar medium, with [C]/[H] gas = (0.1−1.5) × 10 −4 . HD 100546 itself is a λ Boötis star, with solar abundances of C and O but a strong depletion of rockforming elements. In the gas of the T Tauri disk TW Hya, both C and O are strongly underabundant, with [C]/[H] gas = (0.2−5.0)×10 −6 and C/O > 1. We discuss evidence that the gas-phase C and O abundances are high in the warm inner regions of both disks. Our analytical model, including vertical mixing and a grain size distribution, reproduces the observed [C]/[H] gas in the outer disk of TW Hya and allows to make predictions for other systems.

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Fingerprints of giant planets in the photospheres of Herbig stars

Cited by 110 publications

References 73 publications

Cavity and other radial substructures in the disk around HD 97048

Cavity and other radial substructures in the disk around HD 97048

Spiral Arms in Disks: Planets or Gravitational Instability?

Volatile-carbon locking and release in protoplanetary disks

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