Perturbers: SPHERE detection limits to planetary-mass companions in protoplanetary disks

Asensio-Torres, Rubén; Henning, Th.; Cantalloube, F.; Pinilla, P.; Mesa, D.; Garufi, A.; Jorquera, S.; Gratton, R.; Chauvin, G.; Szulágyi, J.; Boekel, R. van; Dong, Ruobing; Marleau, Gabriel-Dominique; Benisty, M.; Villenave, M.; Bergez-Casalou, C.; Desgrange, C.; Janson, Markus; Keppler, M.; Langlois, M.; Ménard, F.; Rickman, E. L.; Stolker, T.; Feldt, M.; Fusco, Thierry; Glück, L.; Pavlov, A.; Ramos, J.

doi:10.1051/0004-6361/202140325

Cited by 49 publications

(41 citation statements)

References 162 publications

(222 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…While our observations are not sensitive to low mass companions, stellar binary companions of high mass ratio, within the field of view of the telescopes (250 mas for the ATs; 60 mas for the UTs), would have been detected in our interferometric observations. The detection limits available from direct imaging data in the inner regions (within transition disk cavities) are in general limited by the complexities of the disk structures and with the uncertainties in the evolutionary models considered, the current estimates are around a few to ∼10 Jupiter masses (Asensio-Torres et al 2021). So far, out of our sample, only PDS70 has directly imaged planets (Keppler et al 2018) while yet-unconfirmed candidate companions were claimed in the cavities of LkCa15 and HD 100546 (Quanz et al 2013;Sallum et al 2015).…”

Section: Discussionmentioning

confidence: 99%

Probing inner and outer disk misalignments in transition disks

Bohn

Benisty

Perraut

et al. 2022

A&A

Self Cite

View full text Add to dashboard Cite

Context. Transition disks are protoplanetary disks with dust-depleted cavities, possibly indicating substantial clearing of their dust content by a massive companion. For several known transition disks, dark regions interpreted as shadows have been observed in scattered light imaging and are hypothesized to originate from misalignments between distinct regions of the disk. Aims. We aim to investigate the presence of misalignments in transition disks. We study the inner disk (<1 au) geometries of a sample of 20 well-known transition disks with Very Large Telescope Interferometer (VLTI) GRAVITY observations and use complementary 12CO and 13CO molecular line archival data from the Atacama Large Millimeter/submillimeter Array (ALMA) to derive the orientation of the outer disk regions (>10 au). Methods. We fit simple parametric models to the visibilities and closure phases of the GRAVITY data to derive the inclination and position angle of the inner disks. The outer disk geometries were derived from Keplerian fits to the ALMA velocity maps and compared to the inner disk constraints. We also predicted the locations of expected shadows for significantly misaligned systems. Results. Our analysis reveals six disks to exhibit significant misalignments between their inner and outer disk structures. The predicted shadow positions agree well with the scattered light images of HD 100453 and HD 142527, and we find supporting evidence for a shadow in the south of the disk around CQ Tau. In the other three targets for which we infer significantly misaligned disks, V1247 Ori, V1366 Ori, and RY Lup, we do not see any evident sign of shadows in the scattered light images. The scattered light shadows observed in DoAr 44, HD 135344 B, and HD 139614 are consistent with our observations, yet the underlying morphology is likely too complex to be described properly by our models and the accuracy achieved by our observations. Conclusions. The combination of near infrared and submillimeter interferometric observations allows us to assess the geometries of the innermost disk regions and those of the outer disk. Whereas we can derive precise constraints on the potential shadow positions for well-resolved inner disks around Herbig Ae/Be stars, the large statistical uncertainties for the marginally resolved inner disks around the T Tauri stars of our sample make it difficult to extract conclusive constraints for the presence of shadows in these systems.

show abstract

Section: Discussionmentioning

confidence: 99%

Probing inner and outer disk misalignments in transition disks

Bohn

Benisty

Perraut

et al. 2022

A&A

Self Cite

View full text Add to dashboard Cite

show abstract

“…However, there has been detection and confirmation of such planets in only one protoplanetary disk so far (PDS70; Keppler et al 2018;Christiaens et al 2019), although the kinematic signatures of potential planets in different systems are encouraging (e.g., HD 163296; Teague et al 2018Teague et al , 2019. Furthermore, analysis of current observational capabilities suggests that several of the proposed planets that explain some of the substructures should have already been detected (e.g., Asensio-Torres et al 2021). This could indicate that planets may not be the universal origin for disk substructures, especially in the case of younger systems.…”

Section: Introductionmentioning

confidence: 99%

Steady-state accretion in magnetized protoplanetary disks

Delage

Okuzumi

Flock

et al. 2022

A&A

View full text Add to dashboard Cite

Context. The transition between magnetorotational instability (MRI)-active and magnetically dead regions corresponds to a sharp change in the disk turbulence level, where pressure maxima may form, hence potentially trapping dust particles and explaining some of the observed disk substructures. Aims. We aim to provide the first building blocks toward a self-consistent approach to assess the dead zone outer edge as a viable location for dust trapping, under the framework of viscously driven accretion. Methods. We present a 1+1D global magnetically driven disk accretion model that captures the essence of the MRI-driven accretion, without resorting to 3D global nonideal magnetohydrodynamic (MHD) simulations. The gas dynamics is assumed to be solely controlled by the MRI and hydrodynamic instabilities. For given stellar and disk parameters, the Shakura–Sunyaev viscosity parameter, α, is determined self-consistently under the adopted framework from detailed considerations of the MRI with nonideal MHD effects (Ohmic resistivity and ambipolar diffusion), accounting for disk heating by stellar irradiation, nonthermal sources of ionization, and dust effects on the ionization chemistry. Additionally, the magnetic field strength is numerically constrained to maximize the MRI activity. Results. We demonstrate the use of our framework by investigating steady-state MRI-driven accretion in a fiducial protoplanetary disk model around a solar-type star. We find that the equilibrium solution displays no pressure maximum at the dead zone outer edge, except if a sufficient amount of dust particles has accumulated there before the disk reaches a steady-state accretion regime. Furthermore, the steady-state accretion solution describes a disk that displays a spatially extended long-lived inner disk gas reservoir (the dead zone) that accretes a few times 10−9 M⊙ yr−1. By conducting a detailed parameter study, we find that the extent to which the MRI can drive efficient accretion is primarily determined by the total disk gas mass, the representative grain size, the vertically integrated dust-to-gas mass ratio, and the stellar X-ray luminosity. Conclusions. A self-consistent time-dependent coupling between gas, dust, stellar evolution models, and our general framework on million-year timescales is required to fully understand the formation of dead zones and their potential to trap dust particles.

show abstract

“…However, to date planets have only been detected in the cavity of one transition disk (PDS 70, Keppler et al 2018;Christiaens et al 2019), while current observational capabilities should already have detected some of the planets inferred to explain the structures of some of them (e.g. Asensio-Torres et al 2021). This questions the universality of planets as the potential origin of the transition-disk-like structures.…”

Section: Introductionmentioning

confidence: 99%

Large gaps and high accretion rates in photoevaporative transition disks with a dead zone

Gárate

Delage

Stadler

et al. 2021

A&A

View full text Add to dashboard Cite

Context. Observations of young stars hosting transition disks show that several of them have high accretion rates, despite their disks presenting extended cavities in their dust component. This represents a challenge for theoretical models, which struggle to reproduce both features simultaneously. Aims. We aim to explore if a disk evolution model, including a dead zone and disk dispersal by X-ray photoevaporation, can explain the high accretion rates and large gaps (or cavities) measured in transition disks. Methods. We implemented a dead zone turbulence profile and a photoevaporative mass-loss profile into numerical simulations of gas and dust. We performed a population synthesis study of the gas component and obtained synthetic images and SEDs of the dust component through radiative transfer calculations. Results. This model results in long-lived inner disks and fast dispersing outer disks that can reproduce both the accretion rates and gap sizes observed in transition disks. For a dead zone of turbulence αdz = 10−4 and an extent rdz = 10 AU, our population synthesis study shows that 63% of our transition disks are still accreting with Ṁg ≥ 10−11 M⊙ yr−1 after opening a gap. Among those accreting transition disks, half display accretion rates higher than 5.0 × 10−10 M⊙ yr−1. The dust component in these disks is distributed in two regions: in a compact inner disk inside the dead zone, and in a ring at the outer edge of the photoevaporative gap, which can be located between 20 and 100 AU. Our radiative transfer calculations show that the disk displays an inner disk and an outer ring in the millimeter continuum, a feature that resembles some of the observed transition disks. Conclusions. A disk model considering X-ray photoevaporative dispersal in combination with dead zones can explain several of the observed properties in transition disks, including the high accretion rates, the large gaps, and a long-lived inner disk at millimeter emission.

show abstract

Perturbers: SPHERE detection limits to planetary-mass companions in protoplanetary disks

Cited by 49 publications

References 162 publications

Probing inner and outer disk misalignments in transition disks

Probing inner and outer disk misalignments in transition disks

Steady-state accretion in magnetized protoplanetary disks

Large gaps and high accretion rates in photoevaporative transition disks with a dead zone

Contact Info

Product

Resources

About