Quasi-steady vortices in protoplanetary disks

Surville, Clément; Barge, P.

doi:10.1051/0004-6361/201424663

Cited by 32 publications

(63 citation statements)

References 33 publications

(41 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Hence, the vortex is introduced at the beginning of the simulations and, in a few rotations, adjusts to a quasi-steady vortex structure that lasts long enough to significantly perturb the motion of the dust particles. Two dimensional vortices are, indeed, quasi-steady gaseous structures that can survive over very long time periods of up to thousands of vortex rotations around the star (Surville & Barge 2015). Their lifetimes in numerical simulations are shorter when dust is included in the A122, page 2 of 10 disk due to the gas drag, but the present simulations show that the vortices can survive long enough to significantly change the dust surface density and to imprint observable structures in the disks.…”

Section: Vortex Modelmentioning

confidence: 58%

“…In our problem the two conditions are satisfied except (i) when the particle size is larger than one centimeter or (ii) when located in the core of the vortex and close to its orbital radius where dust strongly accumulates. The code was previously developed to study the dynamical evolution of protoplanetary disks (Inaba et al 2005;Surville & Barge 2015). It solves the inviscid continuity and Euler equations vertically integrated over the disk thickness.…”

Section: Numerical Simulationsmentioning

confidence: 99%

“…This code, which uses the finite volume method and was first presented in Inaba et al (2005) can maintain high accuracy over large integration periods (Surville & Barge 2015;Surville et al 2016).…”

Section: Numerical Simulationsmentioning

confidence: 99%

See 2 more Smart Citations

Gaps and rings carved by vortices in protoplanetary dust

Barge

Ricci

Carilli

et al. 2017

A&A

Self Cite

View full text Add to dashboard Cite

Context. Large-scale vortices in protoplanetary disks are thought to form and survive for long periods of time. Hence, they can significantly change the global disk evolution and particularly the distribution of the solid particles embedded in the gas, possibly explaining asymmetries and dust concentrations recently observed at submillimeter and millimeter wavelengths. Aims. We investigate the spatial distribution of dust grains using a simple model of protoplanetary disk hosted by a giant gaseous vortex. We explore the dependence of the results on grain size and deduce possible consequences and predictions for observations of the dust thermal emission at submillimeter and millimeter wavelengths. Methods. Global 2D simulations with a bi-fluid code are used to follow the evolution of a single population of solid particles aerodynamically coupled to the gas. Possible observational signatures of the dust thermal emission are obtained using simulators of ALMA and Nest Generation Very Large Array (ngVLA) observations. Results. We find that a giant vortex not only captures dust grains with Stokes number S t < 1 but can also affect the distribution of larger grains (with S t ∼ 1) carving a gap associated with a ring composed of incompletely trapped particles. The results are presented for different particle sizes and associated with their possible signatures in disk observations. Conclusions. Gap clearing in the dust spatial distribution could be due to the interaction with a giant gaseous vortex and their associated spiral waves without the gravitational assistance of a planet. Hence, strong dust concentrations at short sub-mm wavelengths associated with a gap and an irregular ring at longer mm and cm wavelengths could indicate the presence of an unseen gaseous vortex.

show abstract

Section: Vortex Modelmentioning

confidence: 58%

Section: Numerical Simulationsmentioning

confidence: 99%

See 1 more Smart Citation

Gaps and rings carved by vortices in protoplanetary dust

Barge

Ricci

Carilli

et al. 2017

A&A

Self Cite

View full text Add to dashboard Cite

show abstract

“…The connection between hydrodynamic simulations was previously done by taking azimuthally averaged profile of gas obtained in hydrodynamic simulations and performing the dust coagulation calculation in a postprocessing step (Pinilla et al 2012;Carballido et al 2016). Tamfal et al (2018) included a simplified prescription for dust growth in hydrodynamic code RoSSBi (Surville & Barge 2015;Surville et al 2016), where dust is represented by a single fluid but dust size may be different in every cell and is set in a sub-grid algorithm based on the work of Birnstiel et al (2012), and demonstrated that this approach yields significantly different outcome than fixed-size treatment. Vorobyov et al (2018) implemented a similar method, with two dust populations, where dust growth is limited by barriers as proposed by Birnstiel et al (2012).…”

Section: Introductionmentioning

confidence: 99%

Including Dust Coagulation in Hydrodynamic Models of Protoplanetary Disks: Dust Evolution in the Vicinity of a Jupiter-mass Planet

Drążkowska

Birnstiel

et al. 2019

ApJ

View full text Add to dashboard Cite

Dust growth is often neglected when building models of protoplanetary disks due to its complexity and computational expense. However, it does play a major role in shaping the evolution of protoplanetary dust and planet formation. In this paper, we present a numerical model coupling 2-D hydrodynamic evolution of a protoplanetary disk, including a Jupiter-mass planet, and dust coagulation. This is obtained by including multiple dust fluids in a single grid-based hydrodynamic simulation and solving the Smoluchowski equation for dust coagulation on top of solving for the hydrodynamic evolution. We find that fragmentation of dust aggregates trapped in a pressure bump outside of the planetary gap leads to an enhancement in density of small grains. We compare the results obtained from the full coagulation treatment to the commonly used, fixed dust size approach and to previously applied, less computationally intensive methods for including dust coagulation. We find that the full coagulation results cannot be reproduced using the fixed-size treatment, but some can be mimicked using a relatively simple method for estimating the characteristic dust size in every grid cell.

show abstract

“…In this work we employ the finite volume code RoSSBi (Surville & Barge 2015;Surville & Mayer 2018), which uses the fluid approximation to treat both the gas and the dust component of the disk, solving the relevant equations in two dimensions and in cylindrical coordinates. The evolution of the dust and gas surface density (Σ d , Σ g ) is described by the inviscid Euler equations in a cylindrical coordinate system.…”

Section: Two-fluid Simulation Techniquementioning

confidence: 99%

A Subgrid Model for the Growth of Dust Particles in Hydrodynamical Simulations of Protoplanetary Disks

Tamfal

Drążkowska

Mayer

et al. 2018

ApJ

View full text Add to dashboard Cite

We present the first 2D hydrodynamical finite volume simulations in which dust is fully coupled with the gas, including its back-reaction onto it, and at the same time the dust size is evolving according to coagulation and fragmentation based on a sub-grid model. The aim of this analysis is to present the differences occurring when dust evolution is included relative to simulations with fixed dust size, with and without an embedded Jupiter-mass planet that triggers gap formation. We use the two-fluid polar Godunov-type code RoSSBi developed by Surville et al. (2016) combined with a new local sub-grid method for dust evolution based on the model by Birnstiel et al. (2012). We find striking differences between simulations with variable and fixed dust sizes. The timescales for dust depletion differ significantly and yield a completely different evolution of the dust surface density. In general sharp features such as pile-ups of dust in the inner disk and near gap edges, when a massive planet is present, become much weaker. This has important implications on the interpretation of observed substructure in disks, suggesting that the presence of a massive planet does not necessarily cause sharp gaps and rings in the dust component. Also, particles with different dust sizes show a different distribution, pointing to the importance of multi-wavelength synthetic observations in order to compare with observations by ALMA and other instruments. We also find that simulations adopting fixed intermediate particle sizes, in the range 10 −2 − 10 −1 cm, best approximate the surface density evolution seen in simulations with dust evolution.

show abstract

Quasi-steady vortices in protoplanetary disks

Cited by 32 publications

References 33 publications

Gaps and rings carved by vortices in protoplanetary dust

Gaps and rings carved by vortices in protoplanetary dust

Including Dust Coagulation in Hydrodynamic Models of Protoplanetary Disks: Dust Evolution in the Vicinity of a Jupiter-mass Planet

A Subgrid Model for the Growth of Dust Particles in Hydrodynamical Simulations of Protoplanetary Disks

Contact Info

Product

Resources

About