Spiral arms in the protoplanetary disc HD100453 detected with ALMA: evidence for binary–disc interaction and a vertical temperature gradient

Rosotti, Giovanni; Benisty, M.; Juhász, A.; Teague, Richard; Clarke, C. J.; Dominik, C.; Dullemond, C. P.; Klaassen, Pamela; Matrà, Luca; Stolker, T.

doi:10.1093/mnras/stz3090

Cited by 94 publications

(114 citation statements)

References 94 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…So far no clear spiral structures have been found in the dust continuum (or optically thin lines) of CQ Tau that could be used to further distinguish possible launching scenarios, but these could be made accessible with higher spectral and spatial resolution data. Spiral arms have been observed with ALMA in the continuum of several discs, including for example Elias 2-27 (Pérez et al 2016), IM Lup and WaOph 6 (Huang et al 2018), G17.64+0.16 (Maud et al 2019), MWC 758 (Boehler et al 2018;Dong et al 2018), and HD100453 (Rosotti et al 2020b). For the latter, counterparts to the observed NIR spirals (Wagner et al 2015;Benisty et al 2017) were not only found in the dust continuum but also the CO emission, enabling the authors to study the thermal structure of the disc and link the spirals to a known binary companion.…”

Section: Discussionmentioning

confidence: 99%

A highly non-Keplerian protoplanetary disc

Wölfer

Facchini

Kurtovic

et al. 2021

A&A

View full text Add to dashboard Cite

Context. In recent years high-angular-resolution observations have revealed that circumstellar discs appear in a variety of shapes with diverse substructures being ubiquitous. This has given rise to the question of whether these substructures are triggered by planet–disc interactions. Besides direct imaging, one of the most promising methods to distinguish between different disc-shaping mechanisms is to study the kinematics of the gas disc. In particular, the deviations of the rotation profile from Keplerian velocity can be used to probe perturbations in the gas pressure profile that may be caused by embedded (proto-) planets. Aims. In this paper we aim to analyse the gas brightness temperature and kinematics of the transitional disc around the intermediate-mass star CQ Tau in order to resolve and characterise substructure in the gas caused by possible perturbers. Methods. For our analysis we used spatially resolved ALMA observations of the three CO isotopologues 12CO, 13CO, and C18O (J = 2−1) from the disc around CQ Tau. We further extracted robust line centroids for each channel map and fitted a number of Keplerian disc models to the velocity field. Results. The gas kinematics of the CQ Tau disc present non-Keplerian features, showing bent and twisted iso-velocity curves in 12CO and 13CO. Significant spiral structures are detected between ~10 and 180 au in both the brightness temperature and the rotation velocity of 12CO after subtraction of an azimuthally symmetric model, which may be tracing planet–disc interactions with an embedded planet or low-mass companion. We identify three spirals, two in the brightness temperature and one in the velocity residuals, spanning a large azimuth and radial extent. The brightness temperature spirals are morphologically connected to spirals observed in near-infrared scattered light in the same disc, indicating a common origin. Together with the observed large dust and gas cavity, these spiral structures support the hypothesis of a massive embedded companion in the CQ Tau disc.

show abstract

Section: Discussionmentioning

confidence: 99%

A highly non-Keplerian protoplanetary disc

Wölfer

Facchini

Kurtovic

et al. 2021

A&A

View full text Add to dashboard Cite

show abstract

“…However, theoretical models have shown that in addition to binary-disk interactions, several different processes can also drive the generation of spirals in disks, such as a low-mass companion on an orbit inside or outside of the disk (e.g., Dong et al 2015a), gravitational instability (e.g., Dong et al 2015b;Dipierro et al 2015;Nelson & Marzari 2016;Meru et al 2017), or a combination of both (e.g., Pohl et al 2015), as well as temperature fluctuations as a result of shadowing by a warped or misaligned inner disk (e.g., Montesinos et al 2016). In order to discern between the companion and gravitational instability scenario, observations at comparably high resolution of the dust continuum, probing the midplane of the disk, are required (e.g., Rosotti et al 2020). However, we regard the last scenario as rather unlikely because in this case, the spiral arms would be expected to diverge from a location close to where the scatteredlight shadows are located.…”

Section: Spiral Structures As Imprints Of Binary-disk Interactionmentioning

confidence: 99%

Gap, shadows, spirals, and streamers: SPHERE observations of binary-disk interactions in GG Tauri A

Keppler

Penzlin

Benisty

et al. 2020

A&A

View full text Add to dashboard Cite

Context. A large portion of stars is found to be part of binary or higher-order multiple systems. The ubiquity of planets found around single stars raises the question of whether and how planets in binary systems form. Protoplanetary disks are the birthplaces of planets, and characterizing them is crucial in order to understand the planet formation process. Aims. Our goal is to characterize the morphology of the GG Tau A disk, one of the largest and most massive circumbinary disks. We also aim to trace evidence for binary-disk interactions. Methods. We obtained observations in polarized scattered light of GG Tau A using the SPHERE/IRDIS instrument in the H-band filter. We analyzed the observed disk morphology and substructures. We ran 2D hydrodynamical models to simulate the evolution of the circumbinary ring over the lifetime of the disk. Results. The disk and also the cavity and the inner region are highly structured, with several shadowed regions, spiral structures, and streamer-like filaments. Some of these are detected here for the first time. The streamer-like filaments appear to connect the outer ring with the northern arc. Their azimuthal spacing suggests that they may be generated through periodic perturbations by the binary, which tear off material from the inner edge of the outer disk once during each orbit. By comparing observations to hydrodynamical simulations, we find that the main features, in particular, the gap size, but also the spiral and streamer filaments, can be qualitatively explained by the gravitational interactions of a binary with a semimajor axis of ~35 au on an orbit coplanar with the circumbinary ring.

show abstract

“…The Atacama Large Millimeter/Submillimeter Array (ALMA) is rapidly revolutionizing the field of proto-planetary discs thanks to transformational improvements in sensitivity and spatial resolution compared to the previous generation of sub-mm interferometers. One of the most important discoveries of the last few years is the realisation that most proto-planetary discs are not smooth, but have a wide variety of sub-structures such as gaps (ALMA Partnership et al 2015;Andrews et al 2016), spirals (Pérez et al 2016;Boehler et al 2018;Rosotti et al 2020a) and crescents (Casassus et al 2013;van der Marel et al 2013;Cazzoletti et al 2018), at least for what concerns the dust emission.…”

Section: Introductionmentioning

confidence: 99%

High resolution observations of molecular emission lines toward the CI Tau proto-planetary disc: planet-carved gaps or shadowing?

Rosotti

Ilee

Facchini

et al. 2020

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

Recent observations have revealed that most proto-planetary discs show a pattern of bright rings and dark gaps. However, most of the high-resolution observations have focused only on the continuum emission. In this Paper we present high-resolution ALMA band 7 (0.89mm) observations of the disc around the star CI Tau in the 12CO & 13CO J = 3–2 and CS J = 7–6 emission lines. Our recent work demonstrated that the disc around CI Tau contains three gaps and rings in continuum emission, and we look for their counterparts in the gas emission. While we find no counterpart of the third gap and ring in 13CO, the disc has a gap in emission at the location of the second continuum ring (rather than gap). We demonstrate that this is mostly an artefact of the continuum subtraction, although a residual gap still remains after accounting for this effect. Through radiative transfer modelling we propose this is due to the inner disc shadowing the outer parts of the disc and making them colder. This raises a note of caution in mapping high-resolution gas emission lines observations to the gas surface density – while possible, this needs to be done carefully. In contrast to 13CO, CS emission shows instead a ring morphology, most likely due to chemical effects. Finally, we note that 12CO is heavily absorbed by the foreground preventing any morphological study using this line.

show abstract

Spiral arms in the protoplanetary disc HD100453 detected with ALMA: evidence for binary–disc interaction and a vertical temperature gradient

Cited by 94 publications

References 94 publications

A highly non-Keplerian protoplanetary disc

A highly non-Keplerian protoplanetary disc

Gap, shadows, spirals, and streamers: SPHERE observations of binary-disk interactions in GG Tauri A

High resolution observations of molecular emission lines toward the CI Tau proto-planetary disc: planet-carved gaps or shadowing?

Contact Info

Product

Resources

About