On the Interferometric Sizes of Young Stellar Objects

Monnier, John D.; Millan-Gabet, R.

doi:10.1086/342917

Cited by 229 publications

(280 citation statements)

References 30 publications

(74 reference statements)

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“…This scenario also gained support from the first survey-type near-infrared interferometric observations of Herbig Ae/Be stars. Millan-Gabet et al (2001) could measure the characteristic size of many YSO disks, finding that the measured sizes scale roughly with the square-root of the luminosity L of the stellar source (Monnier & Millan-Gabet 2002). Since this is the expected scaling-relation for the location of the dust-sublimation radius (R subl ∝ L 1/2 ), this finding supports the idea that the near-infrared emission is tracing mainly hot material located in a structure at the location of the dust sublimation radius.…”

Section: Introductionsupporting

confidence: 60%

Revealing the sub-AU asymmetries of the inner dust rim in the disk around the Herbig Ae star R Coronae Austrinae

Kraus¹,

Hofmann²,

Malbet

et al. 2009

A&A

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Context. Unveiling the structure of the disks around intermediate-mass pre-main-sequence stars (Herbig Ae/Be stars) is essential for our understanding of the star and planet formation process. In particular, models predict that in the innermost AU around the star, the dust disk forms a "puffed-up" inner rim, which should result in a strongly asymmetric brightness distribution for disks seen under intermediate inclination.Aims. Our aim is to constrain the sub-AU geometry of the inner disk around the Herbig Ae star R CrA and search for the predicted asymmetries. Methods. Using the VLTI/AMBER long-baseline interferometer, we obtained 24 near-infrared (H-and K-band) spectrointerferometric observations on R CrA. Observing with three telescopes in a linear array configuration, each data set samples three equally spaced points in the visibility function, providing direct information about the radial intensity profile. In addition, the observations cover a wide position angle range (∼97 • ), also probing the position angle dependence of the source brightness distribution. Results. In the derived visibility function, we detect the signatures of an extended (Gaussian FWHM ∼ 25 mas) and a compact component (Gaussian FWHM ∼ 5.8 mas), with the compact component contributing about two-thirds of the total flux (both in H-and K-band). The brightness distribution is highly asymmetric, as indicated by the strong closure phases (up to ∼40 • ) and the detected position angle dependence of the visibilities and closure phases. To interpret these asymmetries, we employ various geometric as well as physical models, including a binary model, a skewed ring model, and a puffed-up inner rim model with a vertical or curved rim shape. For the binary and vertical rim model, no acceptable fits could be obtained. On the other hand, the skewed ring model and the curved puffed-up inner rim model allow us to simultaneously reproduce the measured visibilities and closure phases. From these models we derive the location of the dust sublimation radius (∼0.4 AU), the disk inclination angle (∼35 • ), and a north-south disk orientation (PA ∼ 180−190 • ). Our curved puffed-up rim model can reproduce reasonably well the interferometric observables and the SED and suggests a luminosity of ∼29 L and the presence of relatively large ( > ∼ 1.2 μm) Silicate dust grains. Our study also reveals discrepancies between the measured interferometric observables and the puffed-up inner rim models, providing important constraints for future refinements of these theoretical models. Perpendicular to the disk, two bow shock-like structures appear in the associated reflection nebula NGC 6729, suggesting that the detected sub-AU size disk is the driving engine of a large-scale outflow. Conclusions. Detecting, for the first time, strong non-localized asymmetries in the inner regions of a Herbig Ae disk, our study supports the existence of a puffed-up inner rim in YSO disks.

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Section: Introductionsupporting

confidence: 60%

Revealing the sub-AU asymmetries of the inner dust rim in the disk around the Herbig Ae star R Coronae Austrinae

Kraus¹,

Hofmann²,

Malbet

et al. 2009

A&A

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“…Negative values of q imply that the inner rim of the disc is hotter than the rest of the disc, which is expected for debris discs. Our fiducial model predicts temperatures of the disc inner rim near the dust sublimation threshold at the regularly accepted values ranging from ≈ 1200 K for silicate dust particles to ≈ 2000 K for carbon species (Monnier & Millan-Gabet 2002;Kobayashi et al 2009). Very warm inner discs with temperatures related to the expected dust sublimation temperature for typical dust compositions are known to exist around T Tauri stars (e.g.…”

Section: Resultsmentioning

confidence: 63%

Spectral energy distribution simulations of a possible ring structure around the young, red brown dwarf G 196-3 B

Zakhozhay

Osorio

Béjar

et al. 2016

Mon. Not. R. Astron. Soc.

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The origin of the very red optical and infrared colours of intermediate-age (∼10-500 Myr) L-type dwarfs remains unknown. It has been suggested that low-gravity atmospheres containing large amounts of dust may account for the observed reddish nature. We explored an alternative scenario by simulating protoplanetary and debris discs around G 196-3 B, which is an L3 young brown dwarf with a mass of ∼ 15 M Jup and an age in the interval 20-300 Myr. The best-fit solution to G 196-3 B's photometric spectral energy distribution from optical wavelengths through 24 µm corresponds to the combination of an unreddened L3 atmosphere (T eff ≈ 1870 K) and a warm (≈ 1280 K), narrow (≈ 0.07-0.11 R ⊙ ) debris disc located at very close distances (≈ 0.12-0.20 R ⊙ ) from the central brown dwarf. This putative, optically thick, dusty belt, whose presence is compatible with the relatively young system age, would have a mass ≥ 7 × 10 −10 M ⊕ comprised of sub-micron/micron characteristic dusty particles with temperatures close to the sublimation threshold of silicates. Considering the derived global properties of the belt and the disc-to-brown dwarf mass ratio, the dusty ring around G 196-3 B may resemble the rings of Neptune and Jupiter, except for its high temperature and thick vertical height (≈ 6 × 10 3 km). Our inferred debris disc model is able to reproduce G 196-3 B's spectral energy distribution to a satisfactory level of achievement.

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“…Many studies were conducted in the near-infrared to constrain the dust sublimation radius and in the mid-infrared to probe colder material further from the central star. From PTI, IOTA, and Keck aperture masking measurements, Monnier & Millan-Gabet (2002) presented the first statistical study of the near-IR extension of YSO. This work was then completed by Keck-I measurements (Monnier et al 2005) and presented in a more complete review in Dullemond & Monnier (2010).…”

Section: The Formation Of Massive Starsmentioning

confidence: 99%

An interferometric journey around massive stars

Meilland¹,

Stee²

2014

Proc. IAU

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Abstract. Since the construction in the late nineties of modern facilities such as the VLTI or CHARA, interferometry became a key technique to probe massive stars and their oftencomplex circumstellar environments. Over the last decade, the development of a new generation of beam combiners for these facilities enabled major breakthroughs in the understanding of the formation and evolution of massive stars. In this short review, we will present few of these advances concerning young stellar objects, binarity, mass loss, and stellar surfaces.

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On the Interferometric Sizes of Young Stellar Objects

Cited by 229 publications

References 30 publications

Revealing the sub-AU asymmetries of the inner dust rim in the disk around the Herbig Ae star R Coronae Austrinae

Revealing the sub-AU asymmetries of the inner dust rim in the disk around the Herbig Ae star R Coronae Austrinae

Spectral energy distribution simulations of a possible ring structure around the young, red brown dwarf G 196-3 B

An interferometric journey around massive stars

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