Dust trapping around Lagrangian points in protoplanetary disks

Montesinos, Matías; Garrido-Deutelmoser, Juan; Olofsson, Johan; Giuppone, C. A.; Cuadra, Jorge; Bayo, A.; Sucerquia, Mario; Cuello, Nicolás

doi:10.1051/0004-6361/202038758

Cited by 25 publications

(24 citation statements)

References 66 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The dust trapping at L 4 and L 5 does not leave a visible signature in our synthetic image. The existence of these accumulations should depend on the present level of viscosity and the time of evolution of the system as shown in both Montesinos et al (2020) and Rodenkirch et al (2021). Our simulation only covers an evolutionary time of ∼ 100 kyr and might, therefore, overestimate these dust masses if a possible real planetary system has been evolving for longer.…”

Section: Dust Trapping Settling and Diffusionmentioning

confidence: 96%

“…We measure the respective trapped dust masses to be 0.09 m ⊕ and 0.18 m ⊕ , respectively. This trapping has been studied in details by Montesinos et al (2020) with a focus on the origin of the Trojans in the Solar System and by Rodenkirch et al (2021) with a focus on the observability by ALMA as e.g. suggested in the system HD 163296.…”

Section: Density Distributionmentioning

confidence: 99%

See 1 more Smart Citation

The steady-state hydrodynamics of a long-lived disc: planetary system architecture and prospects of observing a circumplanetary disc shadow in V4046$\,$Sgr

Weber,

Casassus,

Pérez

2021

Preprint

View full text Add to dashboard Cite

Recent imaging of the disc around the V4046 Sgr spectroscopic binary revealed concentric regions of dust rings and gaps. The object's proximity and expected equilibrated state due to its old age (>20 Myr) make it a superb testbed for hydrodynamical studies in direct comparison to observations. We employ two-dimensional hydrodynamical simulations of gas and multiple dust species to test whether the observed structure conforms with the presence of giant planets embedded in the disc. We then perform radiative transfer calculations of sky images, which we filter for the telescope response for comparison with near-infrared and millimetre observations. We find that the existing data are in excellent agreement with a flared disc and the presence of two giant planets, at 9 au and 20 au, respectively. The different ring widths are recovered by diffusion-balanced dust trapping within the gas pressure maxima. In our radiative transfer model, the diffusion in vertical direction is reduced in comparison to the radial value by a factor of five to recover the spectral energy distribution. Further, we report a previously unaddressed, azimuthally-confined intensity decrement on the bright inner ring in the near-infrared scattered light observation. Our model shows that this decrement can be explained by a shadow cast by a circumplanetary disc around the same giant planet that creates the inner cavity in the hydrodynamical simulations. We examine the shape of the intensity indentation and discuss the potential characterisation of a giant planet and its associated disc by its projected shadow in scattered light observations.

show abstract

Section: Dust Trapping Settling and Diffusionmentioning

confidence: 96%

Section: Density Distributionmentioning

confidence: 99%

The steady-state hydrodynamics of a long-lived disc: planetary system architecture and prospects of observing a circumplanetary disc shadow in V4046$\,$Sgr

Weber,

Casassus,

Pérez

2021

Preprint

View full text Add to dashboard Cite

show abstract

“…Beyond the RWI-driven vortices, we note that crescentshaped gas structures could be produced, in the coorbital region of a single planet, due to the slow evacuation of gas around the stable Lagrange points. As such, the dust trapping at L 4 and L 5 could leave observable signatures for Jovian masses (Montesinos et al 2020;Rodenkirch et al 2021). The elongated vortices provided by Regime II show comparable morphologies to these works but with the advantage of being a less transient feature.…”

Section: Observational Signaturesmentioning

confidence: 70%

Substructures in Protoplanetary Disks Imprinted by Compact Planetary Systems

Garrido-Deutelmoser

Petrovich

Krapp

et al. 2022

ApJ

Self Cite

View full text Add to dashboard Cite

The substructures observed in protoplanetary disks may be the signposts of embedded planets carving gaps or creating vortices. The inferred masses of these planets often fall in the Jovian regime despite their low abundance compared to lower-mass planets, partly because previous works often assume that a single substructure (a gap or vortex) is caused by a single planet. In this work, we study the possible imprints of compact systems composed of Neptune-like planets (∼10–30 M ⊕) and show that long-standing vortices are a prevalent outcome when their interplanetary separation (Δa) falls below ∼8 times H p—the average disk’s scale height at the planet’s locations. In simulations where a single planet is unable to produce long-lived vortices, two-planet systems can preserve them for at least 5000 orbits in two regimes: (i) fully shared density gaps with elongated vortices around the stable Lagrange points L 4 and L 5 for the most compact planet pairs (Δa ≲ 4.6 H p), and (ii) partially shared gaps for more widely spaced planets (Δa ∼ 4.6–8 H p) forming vortices in a density ring between the planets through the Rossby wave instability. The latter case can produce vortices with a wide range of aspect ratios down to ∼3 and can occur for planets captured into the 3:2 (2:1) mean-motion resonances for disks’ aspects ratios of h ≳ 0.033 (h ≳ 0.057). We suggest that their long lifetimes are sustained by the interaction of spiral density waves launched by the neighboring planets. Overall, our results show that the distinguishing imprint of compact systems with Neptune-mass planets are long-lived vortices inside the density gaps, which in turn are shallower than single-planet gaps for a fixed gap width.

show abstract

“…Beyond the RWI-driven vortices, we note that crescent-shaped gas structures could be produced, in the co-orbital region of a single planet, due to the slow evacuation of gas around the stable Lagrange points. As such, the dust trapping at L 4 and L 5 could leave observable signatures for Jovian masses (Montesinos et al 2020;Rodenkirch et al 2021). The elongated vortices provided by Regime II show comparable morphologies to these works but with the advantage of being a less transient feature.…”

Section: Observational Signaturesmentioning

confidence: 70%

Substructures in protoplanetary disks imprinted by compact planetary systems

Garrido-Deutelmoser,

Petrovich,

Krapp

et al. 2022

Preprint

Self Cite

View full text Add to dashboard Cite

The substructures observed in protoplanetary disks may be the signposts of embedded planets carving gaps or creating vortices. The inferred masses of these planets often fall in the Jovian regime despite their low abundance compared to lower-mass planets, partly because previous works often assume that a single substructure (a gap or vortex) is caused by a single planet. In this work, we study the possible imprints of compact systems composed of Neptune-like planets (∼ 10 − 30 M ⊕ ) and show that longstanding vortices are a prevalent outcome when their inter-planetary separation (∆a) falls below ∼ 8 times H p -the average disk's scale height at the planets locations. In simulations where a single planet is unable to produce long-lived vortices, two-planet systems can preserve them for at least 5, 000 orbits in two regimes: i) fully-shared density gaps with elongated vortices around the stable Lagrange points L 4 and L 5 for the most compact planet pairs (∆a 4.6 H p ); ii) partially-shared gaps for more widely spaced planets (∆a ∼ 4.6 − 8 H p ) forming vortices in a density ring between the planets through the Rossby wave instability. The latter case can produce vortices with a wide range of aspect ratios down to ∼ 3 and can occur for planets captured into the 3:2 (2:1) mean-motion resonances for disk's aspects ratios of h 0.033 (h 0.057). We suggest that their long lifetimes are sustained by the interaction of spiral density waves launched by the neighboring planets. Overall, our results show that distinguishing imprint of compact systems with Neptune-mass planets are long-lived vortices inside the density gaps, which in turn are shallower than single-planet gaps for a fixed gap width.

show abstract

Dust trapping around Lagrangian points in protoplanetary disks

Cited by 25 publications

References 66 publications

The steady-state hydrodynamics of a long-lived disc: planetary system architecture and prospects of observing a circumplanetary disc shadow in V4046$\,$Sgr

The steady-state hydrodynamics of a long-lived disc: planetary system architecture and prospects of observing a circumplanetary disc shadow in V4046$\,$Sgr

Substructures in Protoplanetary Disks Imprinted by Compact Planetary Systems

Substructures in protoplanetary disks imprinted by compact planetary systems

Contact Info

Product

Resources

About