Observation of Circumstellar Disks:

Dutrey, Anne; Étangs, A. Lecavelier des; Augereau, Jean-Charles

doi:10.2307/j.ctv1v7zdq5.12

Cited by 14 publications

(8 citation statements)

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“…The values obtained for the indexes q and p as well as that for the turbulent broadening are also similar to those found in TTs and some HAE (see e.g. Dutrey et al 2004). R Mon is a very young object (age∼10 5 yr) which is still deeply embedded in the molecular cloud.…”

Section: Discussionsupporting

confidence: 84%

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A Keplerian Gaseous Disk around the B0 Star R Monocerotis

Fuente¹,

Alonso-Albi²,

Bachiller³

et al. 2006

ApJ

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We present high angular resolution observations of the circumstellar disk around the massive Herbig Be star R Mon ( ) in the continuum at 2.7 and 1.3 mm and the CO and rotational lines. Onthe basis of the new 1.3 mm continuum image, we estimate a disk mass (gasϩdust) of 0.007 and an outer M , radius of !150 AU. Our CO images are consistent with the existence of a Keplerian rotating gaseous disk around this star. Up to our knowledge, this is the most clear evidence for the existence of Keplerian disks around massive stars reported thus far. The mass and physical characteristics of this disk are similar to those of the more evolved T Tauri stars and indicate a shorter timescale for the evolution and dispersal of circumstellar disks around massive stars which lose most of their mass before the star becomes visible.

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Section: Discussionsupporting

confidence: 84%

“…Moreover, the values of p, q and ∆v turb are similar to those measured in the disks associated with TTs and HAE (see e.g. Dutrey et al 2004) suggesting that all these stars host disks with similar physical characteristics.…”

Section: Compact Component: a Keplerian Gaseous Disksupporting

confidence: 76%

A Keplerian Gaseous Disk around the B0 Star R Monocerotis

Fuente¹,

Alonso-Albi²,

Bachiller³

et al. 2006

ApJ

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“…In addition, a CO gas emission line is also resolved within ∼50 au by Goto et al (2006) with an inner clearing cavity inside 10 au. The gas kinematics indicates that the central part of the disk rotates clockwise and the southeast side is in the front, in agreement with what is inferred from the outer part (Dutrey et al 2004). Attempts in scattered light with differential polarimetry was unsuccessful (Garufi et al 2014, for instance).…”

Section: Introductionsupporting

confidence: 65%

Discovery of concentric broken rings at sub-arcsec separations in the HD 141569A gas-rich, debris disk with VLT/SPHERE

Perrot

Boccaletti

Pantin

et al. 2016

A&A

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Context. Transition disks correspond to a short stage between the young protoplanetary phase and older debris phase. Along this evolutionary sequence, the gas component disappears leaving room for a dust-dominated environment where already-formed planets signpost their gravitational perturbations. Aims. We endeavor to study the very inner region of the well-known and complex debris, but still gas-rich disk, around HD 141569A using the exquisite high-contrast capability of SPHERE at the VLT. Recent near-infrared (IR) images suggest a relatively depleted cavity within ∼200 au, while former mid-IR data indicate the presence of dust at separations shorter than ∼100 au. Methods. We obtained multi-wavelength images in the near-IR in J, H2, H3 and Ks-bands with the IRDIS camera and a 0.95-1.35 µm spectral data cube with the IFS. Data were acquired in pupil-tracking mode, thus allowing for angular differential imaging. Results. We discovered several new structures inside 1 , of which the most prominent is a bright ring with sharp edges (semi-major axis: 0.4 ) featuring a strong north-south brightness asymmetry. Other faint structures are also detected from 0.4 to 1 in the form of concentric ringlets and at least one spiral arm. Finally, the VISIR data at 8.6 µm suggests the presence of an additional dust population closer in. Besides, we do not detect companions more massive than 1-3 mass of Jupiter. Conclusions. The performance of SPHERE allows us to resolve the extended dust component, which was previously detected at thermal and visible wavelengths, into very complex patterns with strong asymmetries; the nature of these asymmetries remains to be understood. Scenarios involving shepherding by planets or dust-gas interactions will have to be tested against these observations.

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“…Such more massive systems should fall into a loosely defined category of "transition" discs between T-Tauri or Herbig Ae protoplanetary systems and "proper" debris discs (see for example Sect. 4 of Dutrey et al 2004). For such systems (of which HD141569 is a typical example), which are younger than the more evolved debris discs, risks (or chances) of encountering large amounts of remaining gas are high.…”

Section: Avalanches In Observed Systems Perspectivesmentioning

confidence: 97%

Collisional dust avalanches in debris discs

Grigorieva¹,

Artymowicz

Thébault

2006

A&A

102

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We quantitatively investigate how collisional avalanches may develop in debris discs as the result of the initial breakup of a planetesimal or comet-like object, triggering a collisional chain reaction due to outward escaping small dust grains. We use a specifically developed numerical code that follows both the spatial distribution of the dust grains and the evolution of their size-frequency distribution due to collisions. We investigate how strongly avalanche propagation depends on different parameters (e.g., amount of dust released in the initial breakup, collisional properties of dust grains, and their distribution in the disc). Our simulations show that avalanches evolve on timescales of ∼1000 years, propagating outwards following a spiral-like pattern, and that their amplitude exponentially depends on the number density of dust grains in the system. We estimate the probability of witnessing an avalanche event as a function of disc densities, for a gas-free case around an A-type star, and find that features created by avalanche propagation can lead to observable asymmetries for dusty systems with a β Pictoris-like dust content or higher. Characteristic observable features include: (i) a brightness asymmetry of the two sides for a disc viewed edge-on, and (ii) a one-armed open spiral or a lumpy structure in the case of face-on orientation. A possible system in which avalanche-induced structures might have been observed is the edge-on seen debris disc around HD 32297, which displays a strong luminosity difference between its two sides.

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Observation of Circumstellar Disks:

Cited by 14 publications

References 0 publications

A Keplerian Gaseous Disk around the B0 Star R Monocerotis

A Keplerian Gaseous Disk around the B0 Star R Monocerotis

Discovery of concentric broken rings at sub-arcsec separations in the HD 141569A gas-rich, debris disk with VLT/SPHERE

Collisional dust avalanches in debris discs

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