Shadows and asymmetries in the T Tauri disk HD 143006: evidence for a misaligned inner disk

Benisty, M.; Juhász, A.; Facchini, Stefano; Pinilla, P.; Boer, J. de; Pérez, Laura; Keppler, M.; Muro-Arena, G. A.; Villenave, M.; Andrews, Sean M.; Dominik, C.; Dullemond, C. P.; Gallenne, A.; Garufi, A.; Ginski, C.; Isella, Andrea

doi:10.1051/0004-6361/201833913

Cited by 115 publications

(122 citation statements)

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“…This hinted toward significantly misaligned inner disc components and/or the need for other dipper mechanisms. Evidence of misaligned inner discs has also been recently inferred for several systems using high-contrast optical/infrared images, which have revealed shadows in the outer disc cast by unseen inclined inner disc components (e.g., Marino et al 2015;Stolker et al 2016;Debes et al 2017; Benisty et al 2018;Casassus et al 2018). A notable example is the dipper J1604, which hosts a face-on transition disc resolved by ALMA (Ansdell et al 2016a) and variable shadows seen by VLT/SPHERE (Pinilla et al 2018a), suggesting a highly misaligned (∼70-90 • ) and dynamic inner disc component.…”

Section: Introductionmentioning

confidence: 82%

Are inner disc misalignments common? ALMA reveals an isotropic outer disc inclination distribution for young dipper stars

Ansdell

Gaidos

Hedges

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Dippers are a common class of young variable star exhibiting day-long dimmings with depths of up to several tens of percent. A standard explanation is that dippers host nearly edge-on (i d ≈ 70 • ) protoplanetary discs that allow close-in (<1 au) dust lifted slightly out of the midplane to partially occult the star. The identification of a face-on dipper disc and growing evidence of inner disc misalignments brings this scenario into question. Thus we uniformly (re)derive the inclinations of 24 dipper discs resolved with (sub-)mm interferometry from ALMA. We find that dipper disc inclinations are consistent with an isotropic distribution over i d ≈ 0 − 75 • , above which the occurrence rate declines (likely an observational selection effect due to optically thick disc midplanes blocking their host stars). These findings indicate that the dipper phenomenon is unrelated to the outer (>10 au) disc resolved by ALMA and that inner disc misalignments may be common during the protoplanetary phase. More than one mechanism may contribute to the dipper phenomenon, including accretion-driven warps and "broken" discs caused by inclined (sub-)stellar or planetary companions.

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Section: Introductionmentioning

confidence: 82%

Are inner disc misalignments common? ALMA reveals an isotropic outer disc inclination distribution for young dipper stars

Ansdell

Gaidos

Hedges

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…When the misalignment between the inner and outer components is large, twin narrow shadows are cast on the surface of the outer disk (Avenhaus et al 2014;Marino et al 2015). For small misalignments, however, when the relative inclination between components is only of a few degrees, a single broad shadow is cast (Juhász & Facchini 2017;Debes et al 2017;Benisty et al 2018). The shape of the asymmetry of the outer disk, with the fainter region of the disk appearing roughly constrained to a constant range of PAs between ∼0 • and 240 • (see Fig.…”

Section: Motivationmentioning

confidence: 99%

Shadowing and multiple rings in the protoplanetary disk of HD 139614

Muro-Arena

Benisty

Ginski

et al. 2020

A&A

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Context. Shadows in scattered light images of protoplanetary disks are a common feature and support the presence of warps or misalignments between disk regions. These warps are possibly due to an inclined (sub-)stellar companion embedded in the disk. Aims. We study the morphology of the protoplanetary disk around the Herbig Ae star HD 139614 based on the first scattered light observations of this disk, which we model with the radiative transfer code MCMax3D. Methods. We obtained J-and H-band observations in polarized scattered light with VLT/SPHERE that show strong azimuthal asymmetries. In the outer disk, beyond ∼30 au, a broad shadow spans a range of ∼240 deg in position angle, in the East. A bright ring at ∼16 au also shows an azimuthally asymmetric brightness, with the faintest side roughly coincidental with the brightest region of the outer disk. Additionally, two arcs are detected at ∼34 au and ∼50 au. We created a simple 4-zone approximation to a warped disk model of HD 139614 in order to qualitatively reproduce these features. The location and misalignment of the disk components were constrained from the shape and location of the shadows they cast. Results. We find that the shadow on the outer disk covers a range of position angle too wide to be explained by a single inner misaligned component. Our model requires a minimum of two separate misaligned zones -or a continuously warped region -to cast this broad shadow on the outer disk. A small misalignment of ∼4 • between adjacent components can reproduce most of the observed shadow features. Conclusions. Multiple misaligned disk zones, potentially mimicing a warp, can explain the observed broad shadows in the HD 139614 disk. A planetary mass companion in the disk, located on an inclined orbit, could be responsible for such a feature and for the dust depleted gap responsible for a dip in the SED.

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“…Numerous radial and azimuthal features such as spirals (Benisty et al 2015(Benisty et al , 2017Pérez et al 2016;Huang et al 2018), shadows (Avenhaus et al 2014;Stolker et al 2016;Benisty et al 2018), gaps (ALMA Partnership et al 2015;Tsukagoshi et al corresponding author: cuellonicolas@gmail.com 2016; Dipierro et al 2018;Andrews et al 2018), warps (Langlois et al 2018;Casassus et al 2018;van der Plas et al 2019), horseshoes (van der Marel et al 2013;Boehler et al 2017), and clumps (Dong et al 2018;Gratton et al 2019) have been reported. Such structures are potential signposts of disc-companion interactions (Dong et al 2015;Price et al 2018b;Poblete et al 2019;Calcino et al 2019, for instance).…”

Section: Introductionmentioning

confidence: 99%

Flybys in protoplanetary discs – II. Observational signatures

Cuello

Louvet

Mentiplay

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Tidal encounters in star clusters perturb discs around young protostars. In Cuello et al. (2019a, Paper I) we detailed the dynamical signatures of a stellar flyby in both gas and dust. Flybys produce warped discs, spirals with evolving pitch angles, increasing accretion rates, and disc truncation. Here we present the corresponding observational signatures of these features in optical/near-infrared scattered light and (sub-) millimeter continuum and CO line emission. Using representative prograde and retrograde encounters for direct comparison, we postprocess hydrodynamical simulations with radiative transfer methods to generate a catalogue of multi-wavelength observations. This provides a reference to identify flybys in recent nearinfrared and sub-millimetre observations (e.g., RW Aur, AS 205, HV Tau & DO Tau, FU Ori, V2775 Ori, and Z CMa).

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Shadows and asymmetries in the T Tauri disk HD 143006: evidence for a misaligned inner disk

Cited by 115 publications

References 95 publications

Are inner disc misalignments common? ALMA reveals an isotropic outer disc inclination distribution for young dipper stars

Are inner disc misalignments common? ALMA reveals an isotropic outer disc inclination distribution for young dipper stars

Shadowing and multiple rings in the protoplanetary disk of HD 139614

Flybys in protoplanetary discs – II. Observational signatures

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