The circumstellar disk of HH 30

Madlener, David; Wolf, S.; Dutrey, Anne; Guilloteau, S.

doi:10.1051/0004-6361/201117615

Cited by 35 publications

(48 citation statements)

References 61 publications

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“…Figure 13 shows the calculated midplane temperature as a function of the radial distance from the center. The determined value for T 100 is very similar to other YSOs such as IM Lupi (Pinte et al 2008), CB 26 (Sauter et al 2009), DG Tau, DG Tau-b, HL Tau (Guilloteau et al 2011), and HH 30 (Madlener et al 2012). …”

Section: Disk Structuresupporting

confidence: 78%

“…Together with the quantity h 0 , these five parameters are used to adjust the disk structure in order to fit the data. This ansatz has already been successfully applied to other edge-on circumstellar disks, such as HH 30 (Madlener et al 2012), CB 26 (Sauter et al 2009), IM Lupi (Pinte et al 2008), HV Tauri C , and HK Tauri (Stapelfeldt et al 1998). Integrating Eq.…”

Section: The Diskmentioning

confidence: 99%

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Vertical settling and radial segregation of large dust grains in the circumstellar disk of the Butterfly Star

Gräfe¹,

Wolf²,

Guilloteau³

et al. 2013

A&A

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Context. Circumstellar disks are considered to be the environment for the formation of planets. The growth of dust grains in these disks is the first step in the core accretion-gas capture planet formation scenario. Indicators and evidence of disk evolution can be traced in spatially resolved images and the spectral energy distribution (SED) of these objects. Aims. We develop a model for the dust phase of the edge-on oriented circumstellar disk of the Butterfly Star which allows one to fit observed multi-wavelength images and the SED simultaneously. Methods. Our model is based on spatially resolved high angular resolution observations at 1.3 mm, 894 μm, 2.07 μm, 1.87 μm, 1.60 μm, and 1.13 μm and an extensively covered SED ranging from 12 μm to 2.7 mm, including a detailed spectrum obtained with the Spitzer Space Telescope in the range from 12 μm to 38 μm. A parameter study based on a grid search method involving the detailed analysis of every parameter was performed to constrain the disk parameters and find the best-fit model for the independent observations. The individual observations were modeled simultaneously, using our continuum radiative transfer code. Results. We derived a model that is capable of reproducing all of the observations of the disk at the same time. We find quantitative evidence for grain growth up to ∼100 μm-sized particles, vertical settling of larger dust grains toward the disk midplane, and radial segregation of the latter toward the central star. Within our best-fit model the large grains have a distribution with a scale height of 3.7 AU at 100 AU and a radial extent of 175 AU compared to a hydrostatic scale height of 6.9 AU at 100 AU and an outer disk radius of 300 AU. Our results are consistent with current theoretical models for the evolution of circumstellar disks and the early stages of planet formation.

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Section: Disk Structuresupporting

confidence: 78%

Section: The Diskmentioning

confidence: 99%

Vertical settling and radial segregation of large dust grains in the circumstellar disk of the Butterfly Star

Gräfe¹,

Wolf²,

Guilloteau³

et al. 2013

A&A

Self Cite

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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: 70%

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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“…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: 98%

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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The circumstellar disk of HH 30

Cited by 35 publications

References 61 publications

Vertical settling and radial segregation of large dust grains in the circumstellar disk of the Butterfly Star

Vertical settling and radial segregation of large dust grains in the circumstellar disk of the Butterfly Star

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

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