Low-mass planets in nearly inviscid disks: numerical treatment

Kley, W.; Mueller, Tobias; Kolb, Stefan M.; Benítez-Llambay, Pablo; Masset, F.

doi:10.1051/0004-6361/201219719

Cited by 29 publications

(21 citation statements)

References 32 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…We also vary the power-law indices p, q to examine the effect of the background potential vorticity and dust-to-gas ratio profiles, and consider the effect numerical resolution. Kley et al (2012). We use NR cells logarithmically spaced in R and N φ cells uniformly spaced in φ.…”

Section: Dusty Disc-planet Interactionmentioning

confidence: 99%

Dusty disc–planet interaction with dust-free simulations

Chen

Lin

2018

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

Protoplanets may be born into dust-rich environments if planetesimals formed through streaming or gravitational instabilities, or if the protoplanetary disc is undergoing mass loss due to disc winds or photoevaporation. Motivated by this possibility, we explore the interaction between low mass planets and dusty protoplanetary discs with focus on disc-planet torques. We implement Lin & Youdin's newly developed, purely hydrodynamic model of dusty gas into the Pluto code to simulate dusty protoplanetary discs with an embedded planet. We find that for imperfectly coupled dust and high metallicity, e.g. Stokes number 10 −3 and dust-to-gas ratio Σ d /Σ g = 0.5, a 'bubble' develops inside the planet's co-orbital region, which introduces unsteadiness in the flow. The resulting disc-planet torques sustain large amplitude oscillations that persists well beyond that in simulations with perfectly coupled dust or low dust-loading, where co-rotation torques are always damped. We show that the desaturation of the co-rotation torques by finite-sized particles is related to potential vorticity generation from the misalignment of dust and gas densities. We briefly discuss possible implications for the orbital evolution of protoplanets in dust-rich discs. We also demonstrate Lin & Youdin's dust-free framework reproduces previous results pertaining to dusty protoplanetary discs, including dust-trapping by pressure bumps, dust settling, and the streaming instability.

show abstract

Section: Dusty Disc-planet Interactionmentioning

confidence: 99%

Dusty disc–planet interaction with dust-free simulations

Chen

Lin

2018

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…Note that setting the boundary conditions to open has no significant effect on the results but increases the computational time due to waves developed near the inner boundary. In planet-bearing models, we use H a  ( ) as the smoothing of the gravitational potential of the planet with an appropriate value of 0.6  = (Kley et al 2012). In our simulations, the star is always at the center of the numerical domain.…”

Section: Hydrodynamic Modelsmentioning

confidence: 99%

Interpreting Brightness Asymmetries in Transition Disks: Vortex at Dead Zone or Planet-carved Gap Edges?

Regály

Juhász

Nehéz

2017

ApJ

View full text Add to dashboard Cite

Recent submillimeter observations show nonaxisymmetric brightness distributions with a horseshoe-like morphology for more than a dozen transition disks. The most-accepted explanation for the observed asymmetries is the accumulation of dust in large-scale vortices. Protoplanetary disks' vortices can form by the excitation of Rossby wave instability in the vicinity of a steep pressure gradient, which can develop at the edges of a giant planet-carved gap or at the edges of an accretionally inactive zone. We studied the formation and evolution of vortices formed in these two distinct scenarios by means of two-dimensional locally isothermal hydrodynamic simulations. We found that the vortex formed at the edge of a planetary gap is short-lived, unless the disk is nearly inviscid. In contrast, the vortex formed at the outer edge of a dead zone is long-lived. The vortex morphology can be significantly different in the two scenarios: the vortex radial and azimuthal extensions are ∼1.5 and ∼3.5 times larger for the dead-zone edge compared to gap models. In some particular cases, the vortex aspect ratios can be similar in the two scenarios; however, the vortex azimuthal extensions can be used to distinguish the vortex formation mechanisms. We calculated predictions for vortex observability in the submillimeter continuum with ALMA. We found that the azimuthal and radial extent of the brightness asymmetry correlates with the vortex formation process within the limitations of α-viscosity prescription.

show abstract

“…However, by their nature 2D simulations can not include information about the vertical dynamics or the dynamics of the material above over below the planet. Analysis and simulations of discs by Müller et al (2012) and Kley et al (2012) showed that in order for the results from 2D simulations to be in agreement to their 3D counterparts, the softening parameter for the gravitational potential (Eqn. 3) must be increased to = 0.7H when self-gravity is not taken into consideration.…”

Section: Simulation Setupmentioning

confidence: 91%

Observable scattered light features from inclined and non-inclined planets embedded in protoplanetary discs

Kloster

Flock

2019

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

Over the last few years instruments such as VLT/SPHERE and Subaru/HiCIAO have been able to take detailed scattered light images of protoplanetary discs. Many of the features observed in these discs are generally suspected to be caused by an embedded planet, and understanding the cause of these features requires detailed theoretical models. In this work we investigate disc–planet interactions using the pluto code to run 2D and 3D hydrodynamic simulations of protoplanetary discs with embedded 30 and 300 M⊕ planets on both an inclined (i = 2.86°) and non-inclined orbit, using an α-viscosity of 4 × 10−3. We produce synthetic scattered light images of these discs at H-band wavelengths using the radiative transfer code radmc3d. We find that while the surface density evolution in 2D and 3D simulations of inclined and non-inclined planets remain fairly similar, their observational appearance is remarkably different. Most of the features seen in the synthetic H-band images are connected to density variations of the disc at around 3.3 scale heights above and below the mid-plane, which emphasizes the need for 3D simulations. Planets on sustained orbital inclinations disrupt the disc’s upper atmosphere and produce radically different observable features and intensity profiles, including shadowing effects and intensity variation of the order of 10–20 times the surrounding background. The vertical optical depth to the disc mid-plane for H-band wavelengths is τ ≈ 20 in the disc gap created by the high-mass planet. We conclude that direct imaging of planets embedded in the disc remains difficult to observe, even for massive planets in the gap.

show abstract

Low-mass planets in nearly inviscid disks: numerical treatment

Cited by 29 publications

References 32 publications

Dusty disc–planet interaction with dust-free simulations

Dusty disc–planet interaction with dust-free simulations

Interpreting Brightness Asymmetries in Transition Disks: Vortex at Dead Zone or Planet-carved Gap Edges?

Observable scattered light features from inclined and non-inclined planets embedded in protoplanetary discs

Contact Info

Product

Resources

About