The circumstellar disc in the Bok globule CB 26

Sauter, J.; Wolf, S.; Launhardt, R.; Padgett, Deborah; Stapelfeldt, K.; Pinte, C.; Duchêne, Gaspard; Ménard, F.; McCabe, C.; Pontoppidan, K. M.; Dunham, Michael M.; Bourke, Tyler L.; Chen, J.-H.

doi:10.1051/0004-6361/200912397

Cited by 54 publications

(113 citation statements)

References 51 publications

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“…The parameters derived for the disk model of this source are comparable to those for other circumstellar disks (M total = 0.07 M , see Madlener et al 2012;Gräfe et al 2011;Sauter et al 2009;Schegerer et al 2008;Wolf et al 2003Wolf et al , 2008. Wolf et al (2003) …”

Section: Appendix A: Atacama Large (Sub)millimeter Arraysupporting

confidence: 69%

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Tracing large-scale structures in circumstellar disks with ALMA

Ruge

Wolf

Uribe

et al. 2013

A&A

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Context. Planets are supposed to form in circumstellar disks. The additional gravitational potential of a planet perturbs the disk and leads to characteristic structures, i.e. spiral waves and gaps, in the disk's density profile. Aims. We perform a large-scale parameter study of the observability of these planet-induced structures in circumstellar disks in the (sub)mm wavelength range for the Atacama Large (Sub)Millimeter Array (ALMA). Methods. On the basis of hydrodynamical and magneto-hydrodynamical simulations of star-disk-planet models, we calculated the disk temperature structure and (sub)mm images of these systems. These were used to derive simulated ALMA images. Because appropriate objects are frequent in the Taurus-Auriga region, we focused on a distance of 140 pc and a declination of ≈20 • . The explored range of star-disk-planet configurations consists of six hydrodynamical simulations (including magnetic fields and different planet masses), nine disk sizes with outer radii ranging from 9 AU to 225 AU, 15 total disk masses in the range between 2.67 × 10 −7 M and 4.10 × 10 −2 M , six different central stars, and two different grain size distributions, resulting in 10 000 disk models.Results. On almost all scales and in particular down to a scale of a few AU, ALMA is able to trace disk structures induced by planet-disk interaction or by the influence of magnetic fields on the wavelength range between 0.4 and 2.0 mm. In most cases, the optimum angular resolution is limited by the sensitivity of ALMA. However, within the range of typical masses of protoplanetary disks (0.1-0.001 M ) the disk mass has a minor impact on the observability. It is possible to resolve disks down to 2.67 × 10 −6 M and trace gaps induced by a planet with Mp M = 0.001 in disks with 2.67 × 10 −4 M with a signal-to-noise ratio greater than three. The central star has a major impact on the observability of gaps, as well as the considered maximum grainsize of the dust in the disk. In general, it is more likely to trace planet-induced gaps in our magnetohydrodynamical disk models, because gaps are wider in the presence of magnetic fields. We also find that zonal flows resulting from magneto-rotational instability (MRI) create gap-like structures in the disk's re-emission radiation, which are observable with ALMA. Conclusions. Through the unprecedented resolution and sensitivity of ALMA in the (sub)mm wavelength range, the expected detailed observations of planet-disk interaction and global disk structures will deepen our understanding of the planet formation and disk evolution process.

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Section: Appendix A: Atacama Large (Sub)millimeter Arraysupporting

confidence: 69%

“…The other dust grain radius range (a ∈ 0.005 μm, 0.25 μm ) represents the interstellar medium (Savage & Mathis 1979), which is important for this study because some young stellar objects (e.g. CB26, Sauter et al 2009) show a lack of large dust particles. The absorption properties of the dust depend on the grain size distribution.…”

Section: Radiative Transfermentioning

confidence: 99%

Tracing large-scale structures in circumstellar disks with ALMA

Ruge

Wolf

Uribe

et al. 2013

A&A

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“…For instance, Szűcs et al (2010) investigated the Spitzer/IRAC and MIPS 24 μm photometries of ∼200 stars in the Chamaeleon I star-forming region and found that disks around lower mass stars (spectral type later than M4.75) are generally flatter than the case of higher mass stars (spectral type earlier than M4.5). Coherent multiwavelength modeling suggests a typical flaring index β ∼ 1.25 for T Tauri disks (Wolf et al 2003;Walker et al 2004;Sauter et al 2009;Madlener et al 2012;Gräfe et al 2013). Harvey et al (2012a) report PACS measurements of about 50 very low-mass stars and brown dwarfs with spectral types ranging from M3 to M9 in nearby regions.…”

Section: The Disk Properties Of the Targetsmentioning

confidence: 99%

“…This model has been successfully used to explain the observed SEDs of a large sample of young stellar objects and brown dwarfs (e.g., Wolf et al 2003;Sauter et al 2009;Harvey et al 2012a). For the dust in the disk, we assume a density structure with a Gaussian vertical profile…”

Section: Sed Modelingmentioning

confidence: 99%

Herschel/PACS view of disks around low-mass stars and brown dwarfs in the TW Hydrae association

Liu

Herczeg

Gong

et al. 2014

A&A

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We conducted Herschel/PACS observations of five very low-mass stars or brown dwarfs located in the TW Hya association with the goal of characterizing the properties of disks in the low stellar mass regime. We detected all five targets at 70 μm and 100 μm and three targets at 160 μm. Our observations, combined with previous photometry from 2MASS, WISE, and SCUBA-2, enabled us to construct spectral energy distributions (SEDs) with extended wavelength coverage. Using sophisticated radiative transfer models, we analyzed the observed SEDs of the five detected objects with a hybrid fitting strategy that combines the model grids and the simulated annealing algorithm and evaluated the constraints on the disk properties via the Bayesian inference method. The modeling suggests that disks around low-mass stars and brown dwarfs are generally flatter than their higher mass counterparts, but the range of disk mass extends to well below the value found in T Tauri stars, and the disk scale heights are comparable in both groups. The inferred disk properties (i.e., disk mass, flaring, and scale height) in the low stellar mass regime are consistent with previous findings from large samples of brown dwarfs and very low-mass stars. We discuss the dependence of disk properties on their host stellar parameters and find a significant correlation between the Herschel far-IR fluxes and the stellar effective temperatures, probably indicating that the scaling between the stellar and disk masses (i.e., M disk ∝ M ) observed mainly in low-mass stars may extend down to the brown dwarf regime.

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“…Conclusions obtained using spectral energy distribution (SED) modeling are much more model-dependent and degenerate than using resolved images. Therefore, imaging of protoplanetary disks provides an independent check of SED modeling and a far less ambiguous method for studying the disk structure (e.g., Eisner et al 2009;Hughes et al 2009;Sauter et al 2009;Madlener et al 2012;Gräfe et al 2013). Various efforts to resolve the inner emission holes through direct imaging observations have been undertaken (e.g.…”

Section: Introductionmentioning

confidence: 99%

Mid-infrared observations of the circumstellar disks around PDS 66 and CRBR 2422.8-3423

Gräfe¹,

Wolf²

2013

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Aims. We present mid-infrared observations and photometry of the circumstellar disks around PDS 66 and CRBR 2422.8-3423, obtained with VISIR/VLT in the N band and for the latter also in the Q band. Our aim is to resolve the inner regions of these protoplanetary disks, which carry potential signatures of intermediate or later stages of disk evolution and ongoing planet formation. Methods. We determined the radial brightness profiles of our target objects and the corresponding PSF reference that were observed before and after our target objects. Background standard deviations, the standard errors, and the seeing variations during the observations were considered. Adopting a simple radiative transfer model based on parameters taken from previous studies, we derived constraints on the inner-disk hole radius of the dust disk. Results. Neither of the circumstellar disks around our science targets are spatially resolved in our observations. However, we are able to constrain the inner-disk hole radius to <15.0 +0.5 −0.5 AU and <10.5 +0.5 −1.0 AU for PDS 66 and CRBR 2422.8-3423, respectively. The photometry we performed yields N-band flux densities of 599 ± 8 mJy for PDS 66 and 130 ± 14 mJy for CRBR 2422.8-3423, as well as a Q-band flux density of 858 ± 109 mJy for CRBR 2422.8-3423.

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The circumstellar disc in the Bok globule CB 26

Cited by 54 publications

References 51 publications

Tracing large-scale structures in circumstellar disks with ALMA

Tracing large-scale structures in circumstellar disks with ALMA

Herschel/PACS view of disks around low-mass stars and brown dwarfs in the TW Hydrae association

Mid-infrared observations of the circumstellar disks around PDS 66 and CRBR 2422.8-3423

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