Resolved Observations of Transition Disks

Casassus, S.

doi:10.1017/pasa.2016.7

Cited by 54 publications

(29 citation statements)

References 157 publications

(338 reference statements)

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“…Casassus 2016;Owen 2016). These represent the fraction of transition discs with large, mm-bright cavities and high mass accretion rates.…”

Section: Discussionmentioning

confidence: 99%

“…In particular, dust horseshoes or rings surrounding the central cavities in mm-bright transition discs appear to be widespread (van der Marel et al 2016;Canovas et al 2016; see review by Casassus 2016), with horseshoes normally interpreted as 'dust traps' caused by a vortex at the edge of a planet-induced gap (e.g. Pinilla et al 2012;van der Marel et al 2013;Baruteau & Zhu 2016;Marino et al 2015b).…”

Section: Danielprice@monashedumentioning

confidence: 99%

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Circumbinary, not transitional: on the spiral arms, cavity, shadows, fast radial flows, streamers, and horseshoe in the HD 142527 disc

Price

Cuello

Pinte

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We present 3D hydrodynamical models of the HD142527 protoplanetary disc, a bright and well studied disc that shows spirals and shadows in scattered light around a 100 au gas cavity, a large horseshoe dust structure in mm continuum emission, together with mysterious fast radial flows and streamers seen in gas kinematics. By considering several possible orbits consistent with the observed arc, we show that all of the main observational features can be explained by one mechanism -the interaction between the disc and the observed binary companion. We find that the spirals, shadows and horseshoe are only produced in the correct position angles by a companion on an inclined and eccentric orbit approaching periastron -the 'red' family from Lacour et al. (2016). Dust-gas simulations show radial and azimuthal concentration of dust around the cavity, consistent with the observed horseshoe. The success of this model in the HD142527 disc suggests other mm-bright transition discs showing cavities, spirals and dust asymmetries may also be explained by the interaction with central companions.

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“…Casassus 2016;Owen 2016). These represent the fraction of transition discs with large, mm-bright cavities and high mass accretion rates.…”

Section: Discussionmentioning

confidence: 99%

Section: Danielprice@monashedumentioning

confidence: 99%

Circumbinary, not transitional: on the spiral arms, cavity, shadows, fast radial flows, streamers, and horseshoe in the HD 142527 disc

Price

Cuello

Pinte

et al. 2018

Monthly Notices of the Royal Astronomical Society

Self Cite

182

199

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“…Shadows due to central warps have often been invoked to account for protoplanetary disk properties(e.g. Casassus 2016), such as the low-amplitude modulation of the HST images in TW Hya (Rosenfeld et al 2012;Debes et al 2017), or disk orientation changes in different angular scales (e.g. as in GM Aur, AB Aur, or MWC 758, Hughes et al 2009;Tang et al 2012;Isella et al 2010).…”

Section: Introductionmentioning

confidence: 99%

An inner warp in the DoAr 44 T Tauri transition disc

Casassus

Avenhaus

Pérez

et al. 2018

Monthly Notices of the Royal Astronomical Society

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Optical/IR images of transition disks (TDs) have revealed deep intensity decrements in the rings of HAeBes HD 142527 and HD 100453, that can be interpreted as shadowing from sharply tilted inner disks, such that the outer disks are directly exposed to stellar light. Here we report similar dips in SPHERE+IRDIS differential polarized imaging (DPI) of TTauri DoAr 44. With a fairly axially symmetric ring in the sub mm radio continuum, DoAr 44 is likely also a warped system. We constrain the warp geometry by comparing radiative transfer predictions with the DPI data in H band (Q φ (H)) and with a re-processing of archival 336 GHz ALMA observations. The observed DPI shadows have coincident radio counterparts, but the intensity drops are much deeper in Q φ (H) (∼88%), compared to the shallow drops at 336 GHz (∼24%). Radiative transfer predictions with an inner disk tilt of ∼ 30 ± 5 deg approximately account for the observations. ALMA long-baseline observations should allow the observation of the warped gas kinematics inside the cavity of DoAr 44.

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“…The advents of the Atacama Large Millimeter Array (ALMA) and extreme adaptive optics high-contrast imaging instruments have recently unveiled a wealth of features in protoplanetary disks, including cavities, rings, spiral arms, warps and asymmetric dust distributions (see Casassus 2016, and references therein). A major challenge now is to connect these observed features to the process of planet formation, which is believed to be con-Based on observations made with ESO Telescopes at the Paranal Observatory under program ID 084.C-0952 and 093.C-0526.…”

Section: Introductionmentioning

confidence: 99%

Characterization of low-mass companion HD 142527 B

Christiaens

Casassus

Absil

et al. 2018

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Context. The circumstellar disk of the Herbig Fe star HD 142527 is host to several remarkable features including a warped inner disk, a 120 au-wide annular gap, a prominent dust trap and several spiral arms. A low-mass companion, HD 142527 B, was also found orbiting the primary star at ∼14 au. Aims. This study aims to better characterize this companion, which could help explain its impact on the peculiar geometry of the disk. Methods. We observed the source with VLT/SINFONI in H+K band in pupil-tracking mode. Data were post-processed with several algorithms based on angular differential imaging (ADI). Results. HD 142527 B is conspicuously re-detected in most spectral channels, which enables us to extract the first medium-resolution spectrum of a low-mass companion within 0 . 1 from its central star. Fitting our spectrum with both template and synthetic spectra suggests that the companion is a young M2.5±1.0 star with an effective temperature of 3500 ± 100 K, possibly surrounded with a hot (1700 K) circum-secondary environment. Pre-main sequence evolutionary tracks provide a mass estimate of 0.34 ± 0.06M , independent of the presence of a hot environment. However, the estimated stellar radius and age do depend on that assumption; we find a radius of 1.37 ± 0.05R (resp. 1.96 ± 0.10R ) and an age of 1.8 +1.2 −0.5 Myr (resp. 0.75 ± 0.25 Myr) in the case of the presence (resp. absence) of a hot environment contributing in H+K. Our new values for the mass and radius of the companion yield a mass accretion rate of 4.1-5.8 ×10 −9 M yr −1 (2-3% that of the primary). Conclusions. We have constrained the physical properties of HD 142527 B, thereby illustrating the potential for SINFONI+ADI to characterize faint close-in companions. The new spectral type makes HD 142527 B a twin of the well-known TW Hya T-Tauri star, and the revision of its mass to higher values further supports its role in shaping the disk.

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Resolved Observations of Transition Disks

Cited by 54 publications

References 157 publications

Circumbinary, not transitional: on the spiral arms, cavity, shadows, fast radial flows, streamers, and horseshoe in the HD 142527 disc

Circumbinary, not transitional: on the spiral arms, cavity, shadows, fast radial flows, streamers, and horseshoe in the HD 142527 disc

An inner warp in the DoAr 44 T Tauri transition disc

Characterization of low-mass companion HD 142527 B

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