Multiple spiral patterns in the transitional disk of HD 100546

Boccaletti, A.; Pantin, E.; Lagrange, Anne-Marie; Augereau, J.-C.; Méheut, H.; Quanz, Sascha P.

doi:10.1051/0004-6361/201322365

Cited by 70 publications

(104 citation statements)

References 49 publications

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“…The default observing mode of SPHERE for exoplanet detection (angular differential imaging, Marois et al 2006), is inappropriate in that case because it causes self-subtraction, which can be problematic when dealing with extended objects like circumstellar discs (Boccaletti et al 2013). Instead, we used the method of reference-star subtraction.…”

Section: Methodsmentioning

confidence: 99%

Signatures of massive collisions in debris discs

Kral

Thébault

Augereau

et al. 2014

A&A

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Context. Violent stochastic collisional events have been invoked as a possible explanation for some debris discs displaying pronounced azimuthal asymmetries or having a luminosity excess exceeding that expected for systems at collisional steady-state. So far, no thorough modelling of the consequences of such stochastic events has been carried out, mainly because of the extreme numerical challenge of coupling the dynamical and collisional evolution of the released dust. Aims. We perform the first fully self-consistent modelling of the aftermath of massive breakups in debris discs. We follow the collisional and dynamical evolution of dust released after the breakup of a Ceres-sized body at 6 AU from its central star. We investigate the duration, magnitude, and spatial structure of the signature left by such a violent event, as well as its observational detectability. Methods. We use the recently developed LIDT-DD code, which handles the coupled collisional and dynamical evolution of debris discs. The main focus is placed on the complex interplay between destructive collisions, Keplerian dynamics, and radiation pressure forces. We use the GRaTer package to estimate the system's luminosity at different wavelengths. Results. The breakup of a Ceres-sized body at 6 AU creates an asymmetric dust disc that is homogenized by the coupled action of collisions and dynamics on a timescale of a few 10 5 years. After a transient period where it is very steep, the particle size distribution in the system relaxes to a collisional steady-state law after ∼10 4 years. The luminosity excess in the breakup's aftermath should be detectable by mid-IR photometry, from a 30 pc distance, over a period of ∼10 6 years that exceeds the duration of the asymmetric phase of the disc (a few 10 5 years). As for the asymmetric structures, we derive synthetic images for the VLT/SPHERE and JWST/MIRI instruments, showing that they should be clearly visible and resolved from a 10 pc distance. Images at 1.6 μm (marginally), 11.4, and 15.5 μm show the inner disc structures, while 23 μm images display the outer disc asymmetries.

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Section: Methodsmentioning

confidence: 99%

Signatures of massive collisions in debris discs

Kral

Thébault

Augereau

et al. 2014

A&A

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“…jects and transition discs include: AB Aur (Hashimoto et al 2011), MWC 758 (Grady et al 2013;Benisty et al 2015), SAO 206462 (Muto et al 2012;Garufi et al 2013;Stolker et al 2016), HD 100546 (Boccaletti et al 2013;Avenhaus et al 2014;Currie et al 2015;Garufi et al 2016;Follette et al 2017), HD 100453 (Wagner et al 2015), AK Sco (Janson et al 2016), Elias 2-27 . Alves et al (2017) have presented observations of the Class I object BHB07-11 with a dense 80-au radius disc surrounded by a lower density disc extending to ≈ 300 au that has spiral structure.…”

Section: Discs Around Single Starsmentioning

confidence: 99%

On the diversity and statistical properties of protostellar discs

Bate

2018

Monthly Notices of the Royal Astronomical Society

301

328

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We present results from the first population synthesis study of protostellar discs. We analyse the evolution and properties of a large sample of protostellar discs formed in a radiation hydrodynamical simulation of star cluster formation. Due to the chaotic nature of the star formation process, we find an enormous diversity of young protostellar discs, including misaligned discs, and discs whose orientations vary with time. Star-disc interactions truncate discs and produce multiple systems. Discs may be destroyed in dynamical encounters and/or through ram-pressure stripping, but reform by later gas accretion. We quantify the distributions of disc mass and radii for protostellar ages up to ≈ 10 5 yrs. For low-mass protostars, disc masses tend to increase with both age and protostellar mass. Disc radii range from of order ten to a few hundred au, grow in size on timescales ∼ < 10 4 yr, and are smaller around lower-mass protostars. The radial surface density profiles of isolated protostellar discs are flatter than the minimum mass solar nebula model, typically scaling as Σ ∝ r −1. Disc to protostar mass ratios rarely exceed two, with a typical range of M d /M * = 0.1−1 to ages ∼ < 10 4 yrs and decreasing thereafter. We quantify the relative orientation angles of circumstellar discs and the orbit of bound pairs of protostars, finding a preference for alignment that strengths with decreasing separation. We also investigate how the orientations of the outer parts of discs differ from the protostellar and inner disc spins for isolated protostars and pairs.

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“…Spiral arms have been observed in scattered light images of several protoplanetary disks, including HD 135344B (Muto et al 2012;Garufi et al 2013;Wahhaj et al 2015), MWC 758 (Grady et al 2013;Benisty et al 2015), HD 100546 (Boccaletti et al 2013;Avenhaus et al 2014b), HD 142527 (Casassus et al 2012;Rameau et al 2012;Canovas et al 2013;Avenhaus et al 2014a), and HD 100453 (Wagner et al 2015). They are caused by local perturbations of the disk surface density and/or scale height but their origin is still under debate.…”

Section: The Origin Of the Spiral Armsmentioning

confidence: 99%

Shadows cast on the transition disk of HD 135344B

Stolker

Dominik

Avenhaus

et al. 2016

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Context. The protoplanetary disk around the F-type star HD 135344B (SAO 206462) is in a transition stage and shows many intriguing structures both in scattered light and thermal (sub-)millimeter emission which are possibly related to planet formation processes. Aims. We aim to study the morphology and surface brightness of the disk in scattered light to gain insight into the innermost disk regions, the formation of protoplanets, planet-disk interactions traced in the surface and midplane layers, and the dust grain properties of the disk surface. Methods. We have carried out high-contrast polarimetric differential imaging (PDI) observations with VLT/SPHERE and obtained polarized scattered light images with ZIMPOL in the R and I-bands and with IRDIS in the Y and J-bands. The scattered light images and surface brightness profiles are used to study in detail structures in the disk surface and brightness variations. We have constructed a 3D radiative transfer model to support the interpretation of several detected shadow features. Results. The scattered light images reveal with unprecedented angular resolution and sensitivity the spiral arms as well as the 25 au cavity of the disk. Multiple shadow features are discovered on the outer disk with one shadow only being present during the second observation epoch. A positive surface brightness gradient is observed in the stellar irradiation corrected (r 2 -scaled) images in southwest direction possibly due to an azimuthally asymmetric perturbation of the temperature and/or surface density by the passing spiral arms. The disk integrated polarized flux, normalized to the stellar flux, shows a positive trend towards longer wavelengths which we attribute to large (2πa λ) aggregate dust grains in the disk surface. Part of the non-azimuthal polarization signal in the U φ image of the J-band observation can be attributed to multiple scattering in the disk. Conclusions. The detected shadow features and their possible variability have the potential to provide insight into the structure of and processes occurring in the innermost disk regions. Possible explanations for the presence of the shadows include a 22 • misaligned inner disk, a warped disk region that connects the inner disk with the outer disk, and variable or transient phenomena such as a perturbation of the inner disk or an asymmetric accretion flow. The spiral arms are best explained by one or multiple protoplanets in the exterior of the disk although no gap is detected beyond the spiral arms up to 1. 0.

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Multiple spiral patterns in the transitional disk of HD 100546

Cited by 70 publications

References 49 publications

Signatures of massive collisions in debris discs

Signatures of massive collisions in debris discs

On the diversity and statistical properties of protostellar discs

Shadows cast on the transition disk of HD 135344B

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