Mid-infrared sizes of circumstellar disks around Herbig Ae/Be stars measured with MIDI on the VLTI

Leinert, Christoph; Boekel, R.J.H.M. van; Waters, L. B. F. M.; Chesneau, O.; Malbet, Fabien; Köhler, Rainer H.; Jaffe, W.; Ratzka, Thorsten; Dutrey, Anne; Preibisch, Thomas; Graser, U.; Bakker, Eric J.; Chagnon, Gilles; Cotton, W. D.; Dominik, C.; Dullemond, C. P.; Glazenborg-Kluttig, Annelie W.; Glindemann, Andreas; Henning, Thomas; Hofmann, K.-H.; Jong, Jeroen de; Lenzen, R.; Ligori, S.; López, B.; Meisner, Jeffrey A.; Morel, S.; Paresce, Francesco; Pel, J. W.; Percheron, Isabelle; Perrin, G.; Przygodda, Frank; Richichi, A.; Schöller, M.; Schuller, P. A.; Stecklum, B.; Ancker, M. E. van den; Lühe, O. von der; Weigelt, G.

doi:10.1051/0004-6361:20047178

Cited by 177 publications

(197 citation statements)

References 33 publications

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“…HD 245185 is the only remaining massive dust disk in the 5 Myr old λ Ori cluster and, based on CO observations, has a very low gas-to-dust mass ratio (Ansdell et al 2015). HD 179218 is a distant (d = 244 pc) group I source that shows evidence of a characteristic dust emission radius that is larger than for group II sources, although a cavity has not definitively been resolved (Leinert et al 2004). …”

Section: Properties Of the Disksmentioning

confidence: 99%

Fingerprints of giant planets in the photospheres of Herbig stars

Kama

Folsom

Pinilla

2015

A&A

111

152

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Around 2% of all A stars have photospheres depleted in refractory elements. This is hypothesised to arise from gas being accreted more efficiently than dust, but the specific processes and the origin of the material -circum-or interstellar -are not known. The same depletion is seen in 30% of young, disk-hosting Herbig Ae/Be stars. We investigate whether the chemical peculiarity originates in a circumstellar disk. Using a sample of systems for which both the stellar abundances and the protoplanetary disk structure are known, we find that stars hosting warm, flaring group I disks typically have Fe, Mg and Si depletions of 0.5 dex compared to the solar-like abundances of stars hosting cold, flat group II disks. The volatile, C and O, abundances in both sets are identical. Group I disks are generally transitional, having radial cavities depleted in millimetre-sized dust grains, while those of group II are usually not. Thus we propose that the depletion of heavy elements emerges as Jupiter-like planets block the accretion of part of the dust, while gas continues to flow towards the central star. We calculate gas to dust ratios for the accreted material and find values consistent with models of disk clearing by planets. Our results suggest that giant planets of ∼0.1 to 10 M Jup are hiding in at least 30% of Herbig Ae/Be disks.

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Section: Properties Of the Disksmentioning

confidence: 99%

Fingerprints of giant planets in the photospheres of Herbig stars

Kama

Folsom

Pinilla

2015

A&A

111

152

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“…We used this method to derive the shape of the surface density profile in the disk wall from the MIDI observations presented in Panić et al (2012) and Leinert et al (2004). The surface density profile directly affects the surface brightness profile and visibility curves (Figs.…”

Section: Figmentioning

confidence: 99%

Planet or brown dwarf? Inferring the companion mass in HD 100546 from the wall shape using mid-infrared interferometry

Mulders

Paardekooper

Panić

et al. 2013

A&A

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Context. Giant planets form in protoplanetary disks while these disks are still gas-rich, and can reveal their presence through the annular gaps they carve out. HD 100546 is a gas-rich disk with a wide gap between a radius of ∼1 and 13 AU, possibly cleared out by a planetary companion or planetary system. Aims. We aim to identify the nature of the unseen companion near the far end of the disk gap. Methods. We used mid-infrared interferometry at multiple baselines to constrain the curvature of the disk wall at the far end of the gap. We used 2D hydrodynamical simulations of embedded planets and brown dwarfs to estimate the viscosity of the disk and the mass of a companion close to the disk wall. Results. We find that the disk wall at the far end of the gap is not vertical, but rounded-off by a gradient in the surface density. This gradient can be reproduced in hydrodynamical simulations with a single, heavy companion ( 30 . . . 80 M Jup ) while the disk has a viscosity of at least α 5 × 10 −3 . Taking into account the changes in the temperature structure after gap opening reduces the lower limit on the planet mass and disk viscosity to 20 M Jup and α = 2 × 10 −3 . Conclusions. The object in the disk gap of HD 100546 that shapes the disk wall is most likely a 60 +20 −40 M Jup brown dwarf, while the disk viscosity is estimated to be at least α = 2 × 10 −3 . The disk viscosity is an important factor in estimating planetary masses from disk morphologies: more viscous disks need heavier planets to open an equally deep gap.

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“…The data presented here were obtained with the mid-IR (8-13 μm) interferometer MIDI (Leinert et al 2003(Leinert et al , 2004 Table 1, showing all 83 individual observations. Six different baseline configurations of two auxiliary telescopes (ATs) were used.…”

Section: Interferometric Observations With Midi/vltimentioning

confidence: 99%

The mid-infrared diameter of W Hydrae

Zhao-Geisler

Quirrenbach

Köhler

et al. 2011

A&A

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Aims. Asymptotic giant branch (AGB) stars are among the largest distributors of dust into the interstellar medium, and it is therefore important to understand the dust formation process and sequence in their strongly pulsating extended atmosphere. By monitoring the AGB star W Hya interferometrically over a few pulsations cycles, the upper atmospheric layers can be studied to obtain information on their chemical gas and dust composition and their intracycle and cycle-to-cycle behavior. Methods. Mid-infrared (8-13 μm) interferometric data of W Hya were obtained with MIDI/VLTI between April 2007 and September 2009, covering nearly three pulsation cycles. The spectrally dispersed visibility data of all 75 observations were analyzed by fitting a circular fully limb-darkened disk (FDD) model to all data and individual pulsation phases. Asymmetries were studied with an elliptical FDD. Results. Modeling results in an apparent angular FDD diameter of W Hya of about (80 ± 1.2) mas (7.8 AU) between 8 and 10 μm, which corresponds to an about 1.9 times larger diameter than the photospheric one. The diameter gradually increases up to (105 ± 1.2) mas (10.3 AU) at 12 μm. In contrast, the FDD relative flux fraction decreases from (0.85 ± 0.02) to (0.77 ± 0.02), reflecting the increased flux contribution from a fully resolved surrounding silicate dust shell. The asymmetric character of the extended structure could be confirmed. An elliptical FDD yields a position angle of (11 ± 20) • and an axis ratio of (0.87 ± 0.07). A weak pulsation dependency is revealed with a diameter increase of (5.4 ± 1.8) mas between visual minimum and maximum, while detected cycle-to-cycle variations are smaller. Conclusions. W Hya's diameter shows a behavior that is very similar to the Mira stars RR Sco and S Ori and can be described by an analogous model. The constant diameter part results from a partially resolved stellar disk, including a close molecular layer of H 2 O, while the increase beyond 10 μm can most likely be attributed to the contribution of a spatially resolved nearby Al 2 O 3 dust shell. Probably due to the low mass-loss rate, close Fe-free silicate dust could not be detected. The results suggest that the formation of amorphous Al 2 O 3 occurs mainly at visual minimum. A possible close Al 2 O 3 dust shell has now been revealed in a few objects calling for self-consistent dynamic atmospheric models including dust formation close to the star. The asymmetry might be explained by an enhanced dust concentration along an N-S axis.

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Mid-infrared sizes of circumstellar disks around Herbig Ae/Be stars measured with MIDI on the VLTI

Cited by 177 publications

References 33 publications

Fingerprints of giant planets in the photospheres of Herbig stars

Fingerprints of giant planets in the photospheres of Herbig stars

Planet or brown dwarf? Inferring the companion mass in HD 100546 from the wall shape using mid-infrared interferometry

The mid-infrared diameter of W Hydrae

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