The Visible and Near‐Infrared Dust Opacity Law in the HH 30 Circumstellar Disk

Watson, A. M.; Stapelfeldt, K.

doi:10.1086/381142

Cited by 39 publications

(63 citation statements)

References 32 publications

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“…This has been suggested by investigations of dust evolution in circumstellar discs where dust grain growth alters the dust grain properties in the circumstellar disc quite considerably whilst it is of less importance in the lowdensity envelope. Evidence for grain growth has been found, for instance, for the circumstellar discs IM Lupi , GG Tau (Duchêne et al 2004;Pinte et al 2007), HH 30 (Watson & Stapelfeldt 2004), IRAS 04302+2247 (Wolf et al 2003), and VV Serpens (Alonso-Albi et al 2008).…”

Section: Article Published By Edp Sciencesmentioning

confidence: 98%

The circumstellar disc in the Bok globule CB 26

Sauter

Wolf²,

Launhardt

et al. 2009

A&A

107

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Context. Circumstellar discs are expected to be the nursery of planets. Grain growth within such discs is the first step in the planet formation process. The Bok globule CB 26 harbours such a young disc. Aims. We present a detailed model of the edge-on circumstellar disc and its envelope in the Bok globule CB 26. Methods. The model is based on HST near-infrared maps in the I, J, H, and K bands, OVRO and SMA radio maps at 1.1 mm, 1.3 mm and 2.7 mm, and the spectral energy distribution (SED) from 0.9 μm to 3 mm. New photometric and spectroscopic data from the Spitzer Space Telescope and the Caltech Submilimeter Observatory are also part of our analysis. Using the self-consistent radiative transfer code MC3D, the model we construct is able to discriminate between parameter sets and dust properties of both envelope and disc. Results. We find that the data are fit by a disc that has an inner hole with a radius of 45 ± 5 AU. Based on a dust model including silicate and graphite, the maximum grain size needed to reproduce the spectral millimetre index is 2.5 μm. Features seen in the nearinfrared images, dominated by scattered light, can be described as a result of a rotating envelope. Conclusions. Successful employment of ISM dust in both the disc and envelope hint that grain growth may not yet play a significant role for the appearance of this system. A large inner hole implies that CB 26 is a circumbinary disc.

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Section: Article Published By Edp Sciencesmentioning

confidence: 98%

The circumstellar disc in the Bok globule CB 26

Sauter

Wolf²,

Launhardt

et al. 2009

A&A

107

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show abstract

“…The large optical color of the disk relative to the star [Á(V À I c ) ¼ 0:8; Krist et al 2002] has been attributed to a combination of reddened illumination by the central starlight on passing through inner circumstellar disks and the scattering characteristics of the dust (Duchêne et al 2004). Observations of edge-on T Tauri stars reveal outflow cavity walls blue in color (relative to their illuminating stars) and whose optical characteristics can be explained by modified ISM extinction laws (Stapelfeldt et al 2003;Watson & Stapelfeldt 2004).…”

Section: The Color Of the Circumstellar Materialsmentioning

confidence: 99%

Hubble Space TelescopeAdvanced Camera for Surveys Coronagraphic Observations of the Dust Surrounding HD 100546

Ardila¹,

Golimowski²,

Krist³

et al. 2007

ApJ

156

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We present HST ACS coronagraphic observations of HD 100546, a B9.5 star, 103 pc away from the Sun, taken in the F435W, F606W, and F814W bands. Scattered light is detected up to 14 00 from the star. The observations are consistent with the presence of an extended flattened nebula with the same inclination as the inner disk. The well-known ''spiral arms'' are clearly observed and trail the rotating disk material. Weaker arms never before reported are also seen. The interarm space becomes brighter, but the structures become more neutral in color at longer wavelengths, which is not consistent with models that assume that they are due to the effects of a warped disk. Along the major disk axis, the colors of the scattered light relative to the star are Á( F435W À F606W ) % 0:0Y0:2 mag and Á( F435W À F814W ) % 0:5Y1 mag. To explain these colors, we explore the role of asymmetric scattering, reddening, and large minimum sizes on ISM-like grains. We conclude that each of these hypotheses by itself cannot explain the colors. The disk colors are similar to those derived for Kuiper Belt objects, suggesting that the same processes responsible for their colors may be at work here. We argue that we are observing only the geometrically thick, optically thin envelope of the disk, while the optically thick disk responsible for the far-IR emission is undetected. The observed spiral arms are then structures on this envelope. The colors indicate that the extended nebulosity is not a remnant of the infalling envelope but reprocessed disk material.

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“…However, as discussed by Watson & Stapelfeldt (2004) the many free parameters of such models are not well constrained by comparisons with the observed energy distributions and continuum light distributions. Observations can be fitted reasonably well with a wide range of dust properties and geometric parameters.…”

Section: Scattering From An Extended Envelope?mentioning

confidence: 99%

Edge-on T Tauri stars

Appenzeller¹,

Bertout

Stahl³

2005

A&A

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Abstract. Using the U echelle spectrograph at the ESO VLT we obtained two-dimensional high-resolution (R = 50 000) spectra of the edge-on disk objects HH30 * , HK Tau B, and HV Tau C. For comparison purposes we also observed with the same equipment both the classical T Tauri star HL Tau and the active late-type star LDN 1551-9. The spectra of all three observed edge-on disks consist of a T Tauri emission and absorption line spectrum with superimposed jet emission lines. Analysis of the spectra confirmed that the disks are completely opaque at visible wavelengths and that light from the central objects reaches us only via scattering layers above and below the disk planes. The central objects of our targets were found to be normal T Tauri stars showing moderate but different amounts of veiling of their photospheric spectra, indicating different accretion rates or evolutionary stages. We suggest that all classical T Tauri stars (CTTSs) show this observed morphology when viewed edge-on.Part of the jet emission from edge-on systems is directly visible to us in the forbidden lines as well as in Hα and He , a finding which contradicts the present paradigm of a pure magnetospheric accretion origin for the formation of hydrogen and helium emission lines in moderately active CTTSs. From a comparison with those Taurus-Auriga CTTSs for which the inclination is reliably known, we conclude that the view angle of CTTS systems is one of the key parameters governing apparent Hα emission strength in the T Tauri class. We discuss the various possible formation regions for the Na  D lines and show that profiles similar to observed ones can be formed at the base of the disk wind.

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The Visible and Near‐Infrared Dust Opacity Law in the HH 30 Circumstellar Disk

Cited by 39 publications

References 32 publications

The circumstellar disc in the Bok globule CB 26

The circumstellar disc in the Bok globule CB 26

Hubble Space TelescopeAdvanced Camera for Surveys Coronagraphic Observations of the Dust Surrounding HD 100546

Edge-on T Tauri stars

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