A comparative study of disc-planet interaction

Val-Borro, M. de; Edgar, Richard G.; Artymowicz, Pawel; Cieciela̧g, P.; Cresswell, Paul; D’Angelo, Gennaro; Delgado-Donate, Eduardo; Dirksen, Gerben; Fromang, Sébastien; Gawryszczak, A.; Klahr, Hubert; Kley, W.; Lyra, Wladimir; Masset, F.; Mellema, Garrelt; Nelson, Richard P.; Paardekooper, Sijme-Jan; Peplinski, Adam; Pierens, A.; Plewa, T.; Rice, Ken; Schäfer, Christoph; Speith, R.

doi:10.1111/j.1365-2966.2006.10488.x

Cited by 411 publications

(448 citation statements)

References 63 publications

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“…We use reflective boundaries for the cylindrical grid and frozen boundaries for the Cartesian grid (Lyra et al 2008a). Both use the buffer zone described in de Val-Borro et al (2006) to damp waves before they reach the boundary. Particles are removed from the simulation if they cross the inner boundary.…”

Section: Initial and Boundary Conditionsmentioning

confidence: 99%

Planet formation bursts at the borders of the dead zone in 2D numerical simulations of circumstellar disks

Lyra¹,

Johansen

Zsom

et al. 2009

A&A

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Context. As accretion in protoplanetary disks is enabled by turbulent viscosity, the border between active and inactive (dead) zones constitutes a location where there is an abrupt change in the accretion flow. The gas accumulation that ensues triggers the Rossby wave instability, which in turn saturates into anticyclonic vortices. It has been suggested that the trapping of solids within them leads to a burst of planet formation on very short timescales. Aims. We study in the formation and evolution of the vortices in greater detail, focusing on the implications for the dynamics of embedded solid particles and planet formation. Methods. We performed two-dimensional global simulations of the dynamics of gas and solids in a non-magnetized thin protoplanetary disk with the Pencil code. We used multiple particle species of radius 1, 10, 30, and 100 cm. We computed the particles' gravitational interaction by a particle-mesh method, translating the particles' number density into surface density and computing the corresponding self-gravitational potential via fast Fourier transforms. The dead zone is modeled as a region of low viscosity. Adiabatic and locally isothermal equations of state are used. Results. The Rossby wave instability is triggered under a variety of conditions, thus making vortex formation a robust process. Inside the vortices, fast accumulation of solids occurs and the particles collapse into objects of planetary mass on timescales as short as five orbits. Because the drag force is size-dependent, aerodynamical sorting ensues within the vortical motion, and the first bound structures formed are composed primarily of similarly-sized particles. In addition to erosion due to ram pressure, we identify gas tides from the massive vortices as a disrupting agent of formed protoplanetary embryos. We find evidence that the backreaction of the drag force from the particles onto the gas modifies the evolution of the Rossby wave instability, with vortices being launched only at later times if this term is excluded from the momentum equation. Even though the gas is not initially gravitationally unstable, the vortices can grow to Q ≈ 1 in locally isothermal runs, which halts the inverse cascade of energy towards smaller wavenumbers. As a result, vortices in models without self-gravity tend to rapidly merge towards a m = 2 or m = 1 mode, while models with self-gravity retain dominant higher order modes (m = 4 or m = 3) for longer times. Non-selfgravitating disks thus show fewer and stronger vortices. We also estimate the collisional velocity history of the particles that compose the most massive embryo by the end of the simulation, finding that the vast majority of them never experienced a collision with another particle at speeds faster than 1 m s −1 . This result lends further support to previous studies showing that vortices provide a favorable environment for planet formation.

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Section: Initial and Boundary Conditionsmentioning

confidence: 99%

Planet formation bursts at the borders of the dead zone in 2D numerical simulations of circumstellar disks

Lyra¹,

Johansen

Zsom

et al. 2009

A&A

Self Cite

168

188

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“…This gives roughly square gridcells throughout the whole domain. At the outer boundary we use damping boundary conditions where the disk profiles are relaxed to the initial profile (de Val-Borro et al 2006). At the inner boundary we use a new type of boundary .…”

Section: A Hydrodynamical Model For Hd 73526mentioning

confidence: 99%

Stability and formation of the resonant system HD 73526

Sándor

Kley²,

Klagyivik

2007

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Context. Based on radial velocity measurements, it has been found that the two giant planets detected around the star HD 73526 are in 2:1 resonance. However, as our numerical integration shows, the derived orbital data for this system result in chaotic behavior of the giant planets, which is uncommon among the resonant extrasolar planetary systems. Aims. We present regular (non-chaotic) orbital solutions for the giant planets in the system HD 73526 and offer formation scenarios based on combining planetary migration and sudden perturbative effects such as planet-planet scattering or rapid dispersal of the protoplanetary disk. A comparison with the already-studied resonant system HD 128311, exhibiting similar behavior, is given. Methods. The new sets of orbital solutions were derived using the Systemic Console. The stability of these solutions was investigated using the Relative Lyapunov indicator, while the migration and scattering effects are studied by gravitational N-body simulations applying non-conservative forces. Additionally, hydrodynamic simulations of embedded planets in protoplanetary disks were performed to follow the capture into resonance. Results. For the system HD 73526 we demonstrate that the observational radial velocity data are consistent with a coplanar planetary system in a stable 2:1 resonance exhibiting apsidal corotation. We have shown that, similarly to the system HD 128311, the present dynamical state of HD 73526 could be the result of a mixed evolutionary process combining planetary migration and a perturbative event.

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“…The other planet-induced structure is a density gap around the orbit of the planet (Goldreich & Tremaine 1980;Papaloizou & Lin 1984). For massive planets, the tidal torques on the surrounding gas overcome the pressure gradient and the viscous spreading, and the gas around the orbital position is pushed away from corotation (Bryden et al 1999;Crida et al 2006;de Val-Borro et al 2006). The density in the gap can be a very small fraction of the initial density.…”

Section: Introductionmentioning

confidence: 99%

Tracing large-scale structures in circumstellar disks with ALMA

Ruge

Wolf

Uribe

et al. 2013

A&A

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Context. Planets are supposed to form in circumstellar disks. The additional gravitational potential of a planet perturbs the disk and leads to characteristic structures, i.e. spiral waves and gaps, in the disk's density profile. Aims. We perform a large-scale parameter study of the observability of these planet-induced structures in circumstellar disks in the (sub)mm wavelength range for the Atacama Large (Sub)Millimeter Array (ALMA). Methods. On the basis of hydrodynamical and magneto-hydrodynamical simulations of star-disk-planet models, we calculated the disk temperature structure and (sub)mm images of these systems. These were used to derive simulated ALMA images. Because appropriate objects are frequent in the Taurus-Auriga region, we focused on a distance of 140 pc and a declination of ≈20 • . The explored range of star-disk-planet configurations consists of six hydrodynamical simulations (including magnetic fields and different planet masses), nine disk sizes with outer radii ranging from 9 AU to 225 AU, 15 total disk masses in the range between 2.67 × 10 −7 M and 4.10 × 10 −2 M , six different central stars, and two different grain size distributions, resulting in 10 000 disk models.Results. On almost all scales and in particular down to a scale of a few AU, ALMA is able to trace disk structures induced by planet-disk interaction or by the influence of magnetic fields on the wavelength range between 0.4 and 2.0 mm. In most cases, the optimum angular resolution is limited by the sensitivity of ALMA. However, within the range of typical masses of protoplanetary disks (0.1-0.001 M ) the disk mass has a minor impact on the observability. It is possible to resolve disks down to 2.67 × 10 −6 M and trace gaps induced by a planet with Mp M = 0.001 in disks with 2.67 × 10 −4 M with a signal-to-noise ratio greater than three. The central star has a major impact on the observability of gaps, as well as the considered maximum grainsize of the dust in the disk. In general, it is more likely to trace planet-induced gaps in our magnetohydrodynamical disk models, because gaps are wider in the presence of magnetic fields. We also find that zonal flows resulting from magneto-rotational instability (MRI) create gap-like structures in the disk's re-emission radiation, which are observable with ALMA. Conclusions. Through the unprecedented resolution and sensitivity of ALMA in the (sub)mm wavelength range, the expected detailed observations of planet-disk interaction and global disk structures will deepen our understanding of the planet formation and disk evolution process.

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A comparative study of disc-planet interaction

Cited by 411 publications

References 63 publications

Planet formation bursts at the borders of the dead zone in 2D numerical simulations of circumstellar disks

Planet formation bursts at the borders of the dead zone in 2D numerical simulations of circumstellar disks

Stability and formation of the resonant system HD 73526

Tracing large-scale structures in circumstellar disks with ALMA

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