Variable Dynamics in the Inner Disk of HD 135344B Revealed with Multi-epoch Scattered Light Imaging<sup>∗</sup>

Stolker, T.; Sitko, Michael L.; Lazareff, B.; Benisty, M.; Dominik, C.; Waters, Rens; Min, M.; Pérez, Sebastián; Milli, J.; Garufi, A.; Boer, J. de; Ginski, C.; Kraus, Stefan; Berger, J.‐P.; Avenhaus, H.

doi:10.3847/1538-4357/aa886a

Cited by 68 publications

(58 citation statements)

References 73 publications

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“…Hashimoto et al 2011;Mayama et al 2012;Avenhaus et al 2014a,b;Garufi et al 2014;Thalmann et al 2015;Akiyama et al 2016;Monnier et al 2017;Bertrang et al 2018), with the new SPHERE / IRDIS instrument being particularly successful at imaging disks at high signal-to-noise ratio (e.g. Pohl et al 2017;Stolker et al 2017). An overview of recent SPHERE results can be found in Garufi et al (2017a).…”

Section: Introductionmentioning

confidence: 99%

Disks around T Tauri Stars with SPHERE (DARTTS-S). I. SPHERE/IRDIS Polarimetric Imaging of Eight Prominent T Tauri Disks*

Avenhaus

Quanz

Garufi

et al. 2018

ApJ

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352

446

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We present the first part of our Disks ARound TTauri Stars with SPHERE (DARTTS-S) survey: observations of eight TTauri stars that were selected based on their strong (sub-)mm excesses using SPHERE / IRDIS polarimetric differential imaging (PDI) in the J and H bands. All observations successfully detect the disks, which appear vastly different in size, from ≈ 80 au in scattered light to >400 au, and display total polarized disk fluxes between 0.06% and 0.89% of the stellar flux. For five of these disks, we are able to determine the three-dimensional structure and the flaring of the disk surface, which appears to be relatively consistent across the different disks, with flaring exponents α between ≈ 1.1 and ≈ 1.6. We also confirm literature results with regard to the inclination and position angle of several of our disks and are able to determine which side is the near side of the disk in most cases. While there is a clear trend of disk mass with stellar ages (≈ 1 Myr to > 10 Myr), no correlations of disk structures with age were found. There are also no correlations with either stellar mass or sub-mm flux. We do not detect significant differences between the J and H bands. However, we note that while a high fraction (7/8) of the disks in our sample show ring-shaped substructures, none of them display spirals, in contrast to the disks around more massive Herbig Ae/Be stars, where spiral features are common.

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Section: Introductionmentioning

confidence: 99%

Disks around T Tauri Stars with SPHERE (DARTTS-S). I. SPHERE/IRDIS Polarimetric Imaging of Eight Prominent T Tauri Disks*

Avenhaus

Quanz

Garufi

et al. 2018

ApJ

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352

446

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“…The reduced Band 3 and Band 4 data (FITS files) are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/ qcat?J/A+A/619/A161 Benisty et al 2015Benisty et al , 2017Pérez et al 2016;Stolker et al 2016Stolker et al , 2017Follette et al 2017;Dong et al 2018) are being observed at mm-wavelength continuum emission with ALMA and in scattered light in the near-infrared (NIR) with VLT/SPHERE (Beuzit et al 2008) and Gemini/GPI (Macintosh et al 2008).…”

Section: Introductionmentioning

confidence: 99%

“…Left panel: ALMA Band 4 observations of HD 135344B at 1.9 mm. Right panel: same image with the contours of the spiral arms observed with SPHERE (Stolker et al 2017) overlaid in white. The panel in the upper left corner shows a zoom into the inner regions, with a colourmap enhancing the emission from the central point-source.…”

Section: Introductionmentioning

confidence: 99%

Evidence for a massive dust-trapping vortex connected to spirals

Cazzoletti

Dishoeck

Pinilla

et al. 2018

A&A

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107

104

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Context. Spiral arms, rings and large scale asymmetries are structures observed in high resolution observations of protoplanetary disks, and it appears that some of the disks showing spiral arms in scattered light also show asymmetries in millimeter-sized dust. HD 135344B is one such disk. Planets are invoked as the origin of these structures, but no planet has been observed so far and upper limits are becoming more stringent with time. Aims. We want to investigate the nature of the asymmetric structure in the HD 135344B disk in order to understand the origin of the spirals and of the asymmetry seen in this disk. Ultimately, we aim to understand whether or not one or more planets are needed to explain such structures. Methods. We present new ALMA sub-0.1′′ resolution observations at optically thin wavelengths (λ = 2.8 and 1.9 mm) of the HD 135344B disk. The high spatial resolution allows us to unambiguously characterize the mm-dust morphology of the disk. The low optical depth of continuum emission probes the bulk of the dust content of the vortex. Moreover, we have combined the new observations with archival data at shorter wavelengths to perform a multi-wavelength analysis and to obtain information about the dust distribution and properties inside the observed asymmetry. Results. We resolve the asymmetric disk into a symmetric ring + asymmetric crescent, and observe that (1) the spectral index strongly decreases at the centre of the vortex, consistent with the presence of large grains; (2) for the first time, an azimuthal shift of the peak of the vortex with wavelength is observed; (3) the azimuthal width of the vortex decreases at longer wavelengths, as expected for dust traps. These features allow confirming the nature of the asymmetry as a vortex. Finally, under the assumption of optically thin emission, a lower limit to the total mass of the vortex is 0.3MJupiter. Considering the uncertainties involved in this estimate, it is possible that the actual mass of the vortex is higher and possibly within the required values (~4 MJupiter) to launch spiral arms similar to those observed in scattered light. If this is the case, then explaining the morphology does not require an outer planet.

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“…Thanks to new capabilities of high resolution instruments such as ALMA, VLT/SPHERE and Gemini/GPI, many features have been identified in protoplanetary disks and in particular in transition disks (TDs). A number of studies reveal rings (e.g., Isella et al 2016;Pohl et al 2017b;Muro-Arena et al 2018), lopsided emission (e.g., Casassus et al 2013;Cazzoletti et al 2018), spirals (e.g., Pérez et al 2016;Dong et al 2018;Muto et al 2012;Stolker et al 2017;Benisty et al 2017;Uyama et al 2018), and shadows (e.g., Marino et al 2015;Stolker et al 2017;Casassus et al 2018;Benisty et al 2018). Among other mechanisms, planets Based on observations performed with SPHERE/VLT under program ID 099.C-0891(A) and 099.C-0147(A).…”

Section: Introductionmentioning

confidence: 99%

Spatial segregation of dust grains in transition disks

Villenave

Benisty

Dent

et al. 2019

A&A

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Context. The mechanisms governing the opening of cavities in transition disks are not fully understood. Several processes have been proposed, but their occurrence rate is still unknown. Aims. We present spatially resolved observations of two transition disks, and aim at constraining their vertical and radial structure using multiwavelength observations that probe different regions of the disks and can help understanding the origin of the cavities. Methods. We have obtained near-infrared scattered light observations with VLT/SPHERE of the transition disks 2MASS J16083070-3828268 (J1608) and RXJ1852.3-3700 (J1852), located in the Lupus and Corona Australis star-forming regions respectively. We complement our datasets with archival ALMA observations, and with unresolved photometric observations covering a wide range of wavelengths. We performed radiative transfer modeling to analyze the morphology of the disks, and then compare the results with a sample of 20 other transition disks observed with both SPHERE and ALMA. Results. We detect scattered light in J1608 and J1852 up to a radius of 0.54′′ and 0.4′′ respectively. The image of J1608 reveals a very inclined disk (i ~ 74°), with two bright lobes and a large cavity. We also marginally detect the scattering surface from the rear-facing side of the disk. J1852 shows an inner ring extending beyond the coronagraphic radius up to 15 au, a gap and a second ring at 42 au. Our radiative transfer model of J1608 indicates that the millimeter-sized grains are less extended vertically and radially than the micron-sized grains, indicating advanced settling and radial drift. We find good agreement with the observations of J1852 with a similar model, but due to the low inclination of the system, the model remains partly degenerate. The analysis of 22 transition disks shows that, in general, the cavities observed in scattered light are smaller than the ones detected at millimeter wavelengths. Conclusions. The analysis of a sample of transition disks indicates that the small grains, well coupled to the gas, can flow inward of the region where millimeter grains are trapped. While 15 out of the 22 cavities in our sample could be explained by a planet of less than 13 Jupiter masses, the others either require the presence of a more massive companion or of several low-mass planets.

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Variable Dynamics in the Inner Disk of HD 135344B Revealed with Multi-epoch Scattered Light Imaging^∗

Cited by 68 publications

References 73 publications

Disks around T Tauri Stars with SPHERE (DARTTS-S). I. SPHERE/IRDIS Polarimetric Imaging of Eight Prominent T Tauri Disks*

Disks around T Tauri Stars with SPHERE (DARTTS-S). I. SPHERE/IRDIS Polarimetric Imaging of Eight Prominent T Tauri Disks*

Evidence for a massive dust-trapping vortex connected to spirals

Spatial segregation of dust grains in transition disks

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Variable Dynamics in the Inner Disk of HD 135344B Revealed with Multi-epoch Scattered Light Imaging∗

Cited by 68 publications

References 73 publications

Disks around T Tauri Stars with SPHERE (DARTTS-S). I. SPHERE/IRDIS Polarimetric Imaging of Eight Prominent T Tauri Disks*

Disks around T Tauri Stars with SPHERE (DARTTS-S). I. SPHERE/IRDIS Polarimetric Imaging of Eight Prominent T Tauri Disks*

Evidence for a massive dust-trapping vortex connected to spirals

Spatial segregation of dust grains in transition disks

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Resources

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Variable Dynamics in the Inner Disk of HD 135344B Revealed with Multi-epoch Scattered Light Imaging^∗