Predicting the Kinematic Evidence of Gravitational Instability

Hall, Cassandra; Dong, Ruobing; Teague, Richard; Terry, Jason; Pinte, C.; Paneque-Carreño, Teresa; Veronesi, Benedetta; Alexander, R. D.; Lodato, Giuseppe

doi:10.3847/1538-4357/abac17

Cited by 44 publications

(45 citation statements)

References 66 publications

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“…Given the small number of spirals, gravitational instability however seems a rather unlikely cause for the spiral structure we observe (e.g. Cossins et al 2009;Hall et al 2020). It is worth considering, nevertheless, that several spiral arms could possibly appear as only two or three arms due to resolution effects (Dipierro et al 2014) and the disc around CQ Tau happens to be relatively massive, therefore gravitational instability cannot be ruled out at this point.…”

Section: Discussionmentioning

confidence: 79%

A highly non-Keplerian protoplanetary disc

Wölfer

Facchini

Kurtovic

et al. 2021

A&A

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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.

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Section: Discussionmentioning

confidence: 79%

A highly non-Keplerian protoplanetary disc

Wölfer

Facchini

Kurtovic

et al. 2021

A&A

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“…Figure 6 shows moment-1 maps with Keplerian rotation subtracted (with each pixel scaled by its distance from the central sink for clarity) for mass ratios of 0.25 and 0.75. Both discs exhibit the "interlocking finger" pattern predicted by Hall et al (2020) as a characteristic imprint of GI. However, the more massive disc, 𝑞 = 0.75, clearly has more pronounced perturbations, strongly suggesting that, when compared to the less massive disc, GI has a larger influence on its dynamics.…”

Section: Discussionmentioning

confidence: 91%

“…However, the origin of the spiral morphology remains unclear. Possibilities that have been investigated include companions, both stellar and planetary, (Dong et al 2015;Fung & Dong 2015;Dong & Fung 2017;Forgan et al 2018b;Price et al 2018b;Huang et al 2018;Dong et al 2018;Veronesi et al 2019;Shen et al 2020) and gravitational instability (GI) , 2005Cossins et al 2009;Dong et al 2015;Hall et al 2016;Meru et al 2017;Forgan et al 2018b;Hall et al 2018;Huang et al 2018;Hall et al 2019Hall et al , 2020Cadman et al 2020b;Chen et al 2021). While it has been demonstrated that GI can be responsible for spiral morphology of some observed discs, it requires the disc-to-star mass ratio, 𝑞, be 0.1 for the spirals to be observable (Cossins et al 2010;Dipierro et al 2014;Dong et al 2015;Hall et al 2016;Kratter & Lodato 2016;Hall et al 2019).…”

Section: Introductionmentioning

confidence: 99%

“…GI) that influence the system evolution (Teague et al 2018;Pinte et al 2018Pinte et al , 2020Hall et al 2020;Disk Dynamics Collaboration et al 2020;Paneque-Carreño et al 2021;Bollati et al 2021;Wölfer et al 2021). It has been shown by Hall et al (2020) that, in contrast to local velocity fluctuations caused by protoplanets, GI-driven spirals should result in global velocity perturbations ("GI wiggles") in molecular line observations. We describe the wiggle in terms of quantifiable parameters, wavelength and amplitude, as shown in Figure 1.…”

Section: Introductionmentioning

confidence: 99%

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Constraining protoplanetary disc mass using the GI wiggle

Terry,

Hall,

Longarini

et al. 2021

Preprint

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Exoplanets form in protoplanetary accretion discs. The total protoplanetary disc mass is the most fundamental parameter, since it sets the mass budget for planet formation. Although observations with the Atacama Large Millimeter/Submillimeter array (ALMA) have dramatically increased our understanding of these discs, total protoplanetary disc mass remains difficult to measure. If a disc is sufficiency massive ( 10% of the host star mass), it can excite gravitational instability (GI). Recently, it has been revealed that GI leaves kinematic imprints of its presence known as the "GI Wiggle." In this work, we use numerical simulations to empirically determine an approximately linear relationship between the amplitude of the wiggle and the host disc-to-star mass ratio, and show that measurements of the amplitude are possible with the spatial and spectral capabilities of ALMA. These measurements can therefore be used to constrain disc-to-star mass ratio.

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“…Although spirals and rings are indications of the existence of planets, they can also possibly result from mechanisms that do not involve planets (e.g., spirals: Dong et al 2015a;Montesinos & Cuello 2018;Hall et al 2020, gaps: Birnstiel et al 2015van der Marel et al 2018). Although the formation of spirals in protoplanetary disks can be caused both with and without planets, the differing mechanisms may be distrinugishable via the structure in the disk.…”

Section: Introductionmentioning

confidence: 99%

Improving Planet Detection with Disk Modeling: Keck/NIRC2 Imaging of the HD 34282 Single-armed Protoplanetary Disk

Quiroz,

Wallack,

Ren

et al. 2021

Preprint

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Formed in protoplanetary disks around young stars, giant planets can leave observational features such as spirals and gaps in their natal disks through planet-disk interactions. Although such features can indicate the existence of giant planets, protoplanetary disk signals can overwhelm the innate luminosity of planets. Therefore, in order to image planets that are embedded in disks, it is necessary to remove the contamination from the disks to reveal the planets possibly hiding within their natal environments. We observe and directly model the detected disk in the Keck/NIRC2 vortex coronagraph L -band observations of the single-armed protoplanetary disk around HD 34282. Despite a non-detection of companions for HD 34282, this direct disk modeling improves planet detection sensitivity by up to a factor of 2 in flux ratio and ∼10 M Jupiter in mass. This suggests that performing disk modeling can improve directly imaged planet detection limits in systems with visible scattered light disks, and can help to better constrain the occurrence rates of self-luminous planets in these systems.

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Predicting the Kinematic Evidence of Gravitational Instability

Cited by 44 publications

References 66 publications

A highly non-Keplerian protoplanetary disc

A highly non-Keplerian protoplanetary disc

Constraining protoplanetary disc mass using the GI wiggle

Improving Planet Detection with Disk Modeling: Keck/NIRC2 Imaging of the HD 34282 Single-armed Protoplanetary Disk

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