The complex structure of the disk around HD 100546

Benisty, M.; Tatulli, E.; Ménard, F.; Swain, Mark R.

doi:10.1051/0004-6361/200913590

Cited by 107 publications

(185 citation statements)

References 31 publications

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“…In such a model, the NIR emission is dominated by the puffed-up inner rim at the dust sublimation radius, and the region of the disk behind the rim is colder owing to shadowing effects, which can lead to a gap in the observed intensity distribution. A gap phenomenon was also reported for other Herbig stars (e.g., Benisty et al 2010;Tatulli et al 2011). While the NIR emission of the disk is dominated exclusively by the inner ring (presumably the puffed-up rim), the MIR emission has a bimodal distribution, with ∼20% of the emission originating from the inner ring, and the rest from the (Monnier & MillanGabet 2002).…”

Section: Discussionsupporting

confidence: 63%

Near-infrared interferometric observation of the Herbig Ae star HD 144432 with VLTI/AMBER

Chen¹,

Kreplin²,

Wang³

et al. 2012

A&A

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Aims. We study the sub-AU-scale circumstellar environment of the Herbig Ae star HD 144432 with near-infrared VLTI/AMBER observations to investigate the structure of its inner dust disk. Methods. The interferometric observations were carried out with the AMBER instrument in the H and K band. We interpret the measured H-and K-band visibilities, the near-and mid-infrared visibilities from the literature, and the spectral energy distribution (SED) of HD 144432 by using geometric ring models and ring-shaped temperature-gradient disk models with power-law temperature distributions.Results. We derive a K-band ring-fit radius of 0.17 ± 0.01 AU and an H-band radius of 0.18 ± 0.01 AU (for a distance of 145 pc). This measured K-band radius of ∼0.17 AU lies in the range between the dust sublimation radius of ∼0.13 AU (predicted for a dust sublimation temperature of 1500 K and gray dust) and the prediction of models including backwarming (∼0.27 AU). We find that an additional extended halo component is required in both the geometric and temperature-gradient modeling. In the best-fit temperaturegradient model, the disk consists of two components. The inner part of the disk is a thin ring with an inner radius of ∼0.21 AU, a temperature of ∼1600 K, and a ring thickness ∼0.02 AU. The outer part extends from ∼1 AU to ∼10 AU with an inner temperature of ∼400 K. We find that the disk is nearly face-on with an inclination angle of <28 • . Conclusions. Our temperature-gradient modeling suggests that the near-infrared excess is dominated by emission from a narrow, bright rim located at the dust sublimation radius, while an extended halo component contributes ∼6% to the total flux at 2 μm. The mid-infrared model emission has a two-component structure with ∼20% of the flux originating from the inner ring and the rest from the outer parts. This two-component structure is indicative of a disk gap, which is possibly caused by the shadow of a puffed-up inner rim.

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Section: Discussionsupporting

confidence: 63%

Near-infrared interferometric observation of the Herbig Ae star HD 144432 with VLTI/AMBER

Chen¹,

Kreplin²,

Wang³

et al. 2012

A&A

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“…However, for an optically thick scattering surface the difference in the radial profiles can be explained with differences in the disk geometry, i.e., stronger disk flaring in HD 97048. And indeed, Benisty et al (2010) A direct comparison between the H-band surface brightness of the two disks reveals that at 60 AU both disks have roughly the same brightness with 13.5 mag/arcsec 2 . At smaller projected separations HD 100546 appears brighter, while at larger separations HD 97048 is brighter.…”

Section: Comparison To Hd 100546mentioning

confidence: 88%

Resolving the inner regions of the HD 97048 circumstellar disk with VLT/NACO polarimetric differential imaging

Quanz

Birkmann

Apai

et al. 2012

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Context. Circumstellar disks are the cradles of planetary systems and their physical and chemical properties directly influence the planet formation process. Because most planets supposedly form in the inner disk regions, i.e., within a few tens of AU, it is crucial to study circumstellar disks on these scales to constrain the conditions for planet formation. Aims. Our aims are to characterize the inner regions of the circumstellar disk around the young Herbig Ae/Be star HD 97048 in polarized light. Methods. We used VLT/NACO to observe HD 97048 in polarimetric differential imaging (PDI) mode in the H and K s band. This technique offers high-contrast capabilities at very small inner working angles and probes the dust grains on the surface layer of the disk that act as the scattering surface. Results. We spatially resolve the disk around HD 97048 in polarized flux in both filters on scales between ∼0.1 -1.0 corresponding to the inner ∼16-160 AU. Fitting isophots to the flux calibrated H-band image between 13-14 mag/arcsec 2 and 14-15 mag/arcsec 2 , we derive an apparent disk inclination angle of 34 • ± 5 • and 47 • ± 2 • , respectively. The disk position angle in both brightness regimes is almost identical and roughly 80 • . Along the disk major axis the surface brightness of the polarized flux drops from ∼11 mag/arcsec 2 at ∼0.1 (∼16 AU) to ∼15.3 mag/arcsec 2 at ∼1.0 (∼160 AU). The brightness profiles along the major axis are fitted with power-laws falling off as ∝r −1.78±0.02 in H and ∝r −2.34±0.04 in K s . Because the surface brightness decreases more rapidly in K s compared to H, the disks becomes relatively bluer at larger separations, possibly indicating changing dust grain properties as a function of radius. Conclusions. We imaged for the first time the inner ∼0.1 -1.0 (∼16-160 AU) of the surface layer of the HD 97048 circumstellar disk in scattered light, which demonstrates the power of ground-based imaging polarimetry. Our data fill an important gap in a large collection of existing data that include resolved thermal dust and polycyclic aromatic hydrocarbon (PAH) emission and also resolved gas emission lines. HD 97048 therefore is an ideal test case for sophisticated models of circumstellar disks and a prime target for future high-contrast imaging observations.

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“…Based on the mid-to near-IR excess ratio, Bouwman et al (2003) suggested an inner cavity in the disk. Later observations confirmed this gap (e.g., Grady et al 2005;Benisty et al 2010). This remarkable feature and the longevity of the HD 100546 disk may point to a young planet in the inner 10 AU, making it a prime target for detailed studies.…”

Section: Introductionmentioning

confidence: 84%

First results of theHerschelkey program “Dust, Ice and Gas In Time” (DIGIT): Dust and gas spectroscopy of HD 100546

Sturm¹,

Bouwman²,

Henning³

et al. 2010

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Context. We present far-infrared spectroscopic observations, taken with the Photodetector Array Camera and Spectrometer (PACS) on the Herschel Space Observatory, of the protoplanetary disk around the pre-main-sequence star HD 100546. These observations are the first within the DIGIT Herschel key program, which aims to follow the evolution of dust, ice, and gas from young stellar objects still embedded in their parental molecular cloud core, through the final pre-main-sequence phases when the circumstellar disks are dissipated. Aims. Our aim is to improve the constraints on temperature and chemical composition of the crystalline olivines in the disk of HD 100546 and to give an inventory of the gas lines present in its far-infrared spectrum. Methods. The 69 μm feature is analyzed in terms of position and shape to derive the dust temperature and composition. Furthermore, we detected 32 emission lines from five gaseous species and measured their line fluxes. Results. The 69 μm emission comes either from dust grains with ∼70 K at radii larger than 50 AU, as suggested by blackbody fitting, or it arises from ∼200 K dust at ∼13 AU, close to the midplane, as supported by radiative transfer models. We also conclude that the forsterite crystals have few defects and contain at most a few percent iron by mass. Forbidden line emission from [C ii] at 157 μm and [O i] at 63 and 145 μm, most likely due to photodissociation by stellar photons, is detected. Furthermore, five H 2 O and several OH lines are detected. We also found high-J rotational transition lines of CO, with rotational temperatures of ∼300 K for the transitions up to J = 22−21 and T ∼ 800 K for higher transitions.

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The complex structure of the disk around HD 100546

Cited by 107 publications

References 31 publications

Near-infrared interferometric observation of the Herbig Ae star HD 144432 with VLTI/AMBER

Near-infrared interferometric observation of the Herbig Ae star HD 144432 with VLTI/AMBER

Resolving the inner regions of the HD 97048 circumstellar disk with VLT/NACO polarimetric differential imaging

First results of theHerschelkey program “Dust, Ice and Gas In Time” (DIGIT): Dust and gas spectroscopy of HD 100546

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