Moving shadows on the dusty disks of young stars

Тамбовцева, Л. В.; Гринин, В. П.; Weigelt, G.

doi:10.1051/0004-6361:20053884

Cited by 7 publications

(13 citation statements)

References 34 publications

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“…An extended low-density atmosphere could be supported by the magnetic field of the inner disk which may explain a large near-infrared excess and possible shadowing (Turner et al 2014). Alternatively, the central star could drive a wind from the circumplanetary disk of a planetary companion (Tambovtseva et al 2006) or disk perturbations by a companion on an inclined orbit may also cause an asymmetric illumination of the disk (Demidova et al 2013). Three-dimensional radiation nonideal magnetohydrodynamical simulations show turbulent velocities in the inner disk up to 10% of the sound speed and a nonaxisymmetric shadow on the outer disk cast by a dead zone-induced vortex (Flock et al 2017).…”

Section: Inner Disk Processes Affecting the Dust Dynamicsmentioning

confidence: 99%

Variable Dynamics in the Inner Disk of HD 135344B Revealed with Multi-epoch Scattered Light Imaging^∗

Stolker

Sitko

Lazareff

et al. 2017

ApJ

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We present multi-epoch Very Large Telescope/Spectro-Polarimetric High-contrast Exoplanet REsearch observations of the protoplanetary disk around HD 135344B (SAO 206462). The J-band scattered light imagery reveal, with high spatial resolution (∼41 mas, 6.4 au), the disk surface beyond ∼20 au. Temporal variations are identified in the azimuthal brightness distributions of all epochs, presumably related to the asymmetrically shading dust distribution in the inner disk. These shadows manifest themselves as narrow lanes, cast by localized density enhancements, and broader features which possibly trace the larger scale dynamics of the inner disk. We acquired visible and near-infrared photometry which shows variations up to 10% in the JHK bands, possibly correlated with the presence of the shadows. Analysis of archival Very Large Telescope Interferometer/PIONIER H-band visibilities constrain the orientation of the inner disk to i = 18.• 2 +3.4−4.1 and PA = 57.• 3 ± 5.• 7, consistent with an alignment with the outer disk or a minor disk warp of several degrees. The latter scenario could explain the broad, quasi-stationary shadowing in N-NW direction in case the inclination of the outer disk is slightly larger. The correlation between the shadowing and the near-infrared excess is quantified with a grid of radiative transfer models. The variability of the scattered light contrast requires extended variations in the inner disk atmosphere (H/r 0.2). Possible mechanisms that may cause asymmetric variations in the optical depth (∆τ 1) through the atmosphere of the inner disk include turbulent fluctuations, planetesimal collisions, or a dusty disk wind, possibly enhanced by a minor disk warp. A fine temporal sampling is required to follow day-to-day changes of the shadow patterns which may be a face-on variant of the UX Orionis phenomenon.

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Section: Inner Disk Processes Affecting the Dust Dynamicsmentioning

confidence: 99%

Variable Dynamics in the Inner Disk of HD 135344B Revealed with Multi-epoch Scattered Light Imaging^∗

Stolker

Sitko

Lazareff

et al. 2017

ApJ

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“…Again, we decided not to increase the complexity of the model without additional observational data supporting this claim because other scenarios such as disk warps, shadowing, and asymmetric illumination by a binary (e.g. Tambovtseva et al 2006) may cause the same effect. The models of B96 and C01 are the counterparts of model A because these studies used optical and NIR observations as the basis for modeling.…”

Section: Fitting Of Nir Observationsmentioning

confidence: 99%

The circumstellar disk of HH 30

Madlener

Wolf

Dutrey

et al. 2012

A&A

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Context. Circumstellar disks are characteristic for star formation and vanish during the first few Myr of stellar evolution. During this time planets are believed to form in the dense midplane by growth, sedimentation and aggregation of dust. Indicators of disk evolution, such as holes and gaps, can be traced in the spectral energy distribution (SED) and spatially resolved images. Aims. We aim to construct a self-consistent model of HH 30 by fitting all available continuum observations simultaneously. New data sets not available in previous studies, such as high-resolution interferometric imaging with the Plateau de Bure Interferometer (PdBI) at λ = 1.3 mm and SED measured with IRS on the Spitzer Space Telescope in the mid-infrared, put strong constraints on predictions and are likely to provide new insights into the evolutionary state of this object. Methods. A parameter study based on simulated annealing was performed to find unbiased best-fit models for independent observations made in the wavelength domain λ ∼ 1 μm . . . 4 mm. The method essentially creates a Markov chain through parameter space by comparing predictions generated by our self-consistent continuum radiation transfer code MC3D with observations. Results. We present models of the edge-on circumstellar disk of HH 30 based on observations from the near-infrared to mmwavelengths that suggest the presence of an inner depletion zone with ∼45 AU radius and a steep decline of mm opacity beyond 140 AU. Our modeling indicates that several modes of dust evolution such as growth, settling, and radial migration are taking place in this object. Conclusions. High-resolution observations of HH 30 at different wavelengths with next-generation observatories such as ALMA and JWST will enable the modeling of inhomogeneous dust properties and significantly expand our understanding of circumstellar disk evolution.

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“…The change of the strength ratio between the violet and red peaks could reflect the relative contribution of the approaching and receding parts of the disk in the different spectra. More sophisticated accretion disk models have recently been developed by Tambovtseva & Grinin (2000) to explain the hydrogen lines of HAeBe stars in a context similar to the widely accepted magnetospheric accretion models for the low-mass T Tauri stars. 2001), ( 5) Penprase (1992), (6) Coulson et al (1998) Fig.…”

Section: Spectroscopymentioning

confidence: 99%

Study of the properties and spectral energy distributions of the Herbig AeBe stars HD 34282 and HD 141569

Merın

Montesinos

Eiroa

et al. 2004

A&A

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Abstract. We present a study of the stellar parameters, distances and spectral energy distributions (SEDs) of HD 34282 and HD 141569, two pre-main sequence Herbig AeBe stars. Both objects have been reported to show "anomalous positions" in the HR diagram in the sense that they appear below the main sequence. A significant result of this work is that both stars are metal-deficient. The Hipparcos distance of HD 34282 is very uncertain and the current study places the star at the expected evolutionary position in the HR diagram, i.e. as a PMS star. The distance for HD 141569 found in this work matches the Hipparcos distance, and the problem of its anomalous position is solved as a result of the low metallicity of the object: using the right metallicity tracks, the star is in the PMS region. The SEDs are constructed using data covering ultraviolet to millimetre wavelengths. Physical, non-parametric models, have been applied in order to extract some properties of the disks surrounding the stars. The disk around HD 34282 is accreting actively, it is massive and presents large grains in the mid-plane and small grains in the surface. HD 141569 has a very low mass disk, which is in an intermediate stage towards a debris-type disk.

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Moving shadows on the dusty disks of young stars

Cited by 7 publications

References 34 publications

Variable Dynamics in the Inner Disk of HD 135344B Revealed with Multi-epoch Scattered Light Imaging^∗

Variable Dynamics in the Inner Disk of HD 135344B Revealed with Multi-epoch Scattered Light Imaging^∗

The circumstellar disk of HH 30

Study of the properties and spectral energy distributions of the Herbig AeBe stars HD 34282 and HD 141569

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Moving shadows on the dusty disks of young stars

Cited by 7 publications

References 34 publications

Variable Dynamics in the Inner Disk of HD 135344B Revealed with Multi-epoch Scattered Light Imaging∗

Variable Dynamics in the Inner Disk of HD 135344B Revealed with Multi-epoch Scattered Light Imaging∗

The circumstellar disk of HH 30

Study of the properties and spectral energy distributions of the Herbig AeBe stars HD 34282 and HD 141569

Contact Info

Product

Resources

About

Variable Dynamics in the Inner Disk of HD 135344B Revealed with Multi-epoch Scattered Light Imaging^∗

Variable Dynamics in the Inner Disk of HD 135344B Revealed with Multi-epoch Scattered Light Imaging^∗