Modelling circumbinary protoplanetary disks

Lines, Stefan; Leinhardt, Z. M.; Baruteau, C.; Paardekooper, Sijme-Jan; Carter, Philip J.

doi:10.1051/0004-6361/201526295

Cited by 31 publications

(37 citation statements)

References 36 publications

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“…In simulations concerning circumbinary planets mainly two types of boundary conditions are used: a closed inner boundary (Pierens & Nelson 2013;Lines et al 2015) that does not allow for mass flow onto the central binary, and outflow boundaries (Kley & Haghighipour 2014 that do allow for accretion onto the binary. While Lines et al (2015) do not find a significant difference between these two case, Kley & Haghighipour (2014) see clear impact on the surface density profile and additionally they were able to construct disks with (on average) constant mass flow through the disk which is not possible for closed boundaries. Driven by these discussions in the literature we decided to perform dedicated numerical studies to test the impact of the location of R min , the chosen boundary condition and other numerical aspects in more detail.…”

Section: Arxiv:170408130v1 [Astro-phep] 26 Apr 2017mentioning

confidence: 99%

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Circumbinary discs: Numerical and physical behaviour

Thun

Kley

Picogna

2017

A&A

139

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Aims. Disks around a central binary system play an important role in star and planet formation as well as for the evolution of galactic disks. These circumbinary disks are strongly disturbed by the time varying potential of the binary system and display a complex dynamical evolution that is not well understood. Our goal is to investigate the impact of disk and binary parameters to the dynamical aspects of the disk. Methods. We study the evolution of circumbinary disks under the gravitational influence of the binary using two-dimensional hydrodynamical simulations. To distinguish between physical and numerical effects we apply three hydrodynamical codes. First we analyse in detail numerical issues concerning the conditions at the boundaries and grid resolution. We then perform a series of simulations with different binary (eccentricity, mass ratio) and disk parameters (viscosity, aspect ratio) starting from a reference model with Kepler-16 parameter.Results. Concerning the numerical aspects we find that the inner grid radius must be of the order of the binary semi-major axis, with free outflow conditions applied such that mass can flow onto the central binary. A closed inner boundary leads to unstable evolutions. We find that the inner disk turns eccentric and precesses for all investigated physical parameters. The precession rate is slow with periods (T prec ) starting at around 500 binary orbits (T bin ) for high viscosity and large H/R where the inner hole is smaller and more circular. Reducing α and H/R increases the gap size and T prec reaches 2500 T bin . For varying binary mass ratios q bin the gap size remains constant whereas T prec decreases for increasing q bin . For varying binary eccentricities e bin we find two separate branches in the gap size and eccentricity diagram. The bifurcation occurs at around e crit ≈ 0.18 where the gap is smallest with the shortest T prec . For e bin smaller and larger than e crit the gap size and T prec increase. Circular binaries create the most eccentric disks.

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Section: Arxiv:170408130v1 [Astro-phep] 26 Apr 2017mentioning

confidence: 99%

“…For the initial disk setup we follow Lines et al (2015). The initial surface density in all our models is given by…”

Section: Initial Disk Parametersmentioning

confidence: 99%

Circumbinary discs: Numerical and physical behaviour

Thun

Kley

Picogna

2017

A&A

139

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“…Our work ties together the pure N-body planetesimal dynamics and growth of Lines et al (2014) and the hydrodynamical simulations of circumbinary gas disks of Lines et al (2015). The work is comparable to that of Marzari et al (2013) who investigate the effects of gas disk gravity on the ability for planetesimal to accumulate in the Kepler-16 system.…”

Section: Discussionmentioning

confidence: 93%

“…These fluid parameters are typical of circumbinary disk simulations. Self-gravitating gas disk simulations are ignored, since Lines et al (2015) found that the gas disk only gravitationally interacts with itself for Σ disk ≥ 2.5 × 10 −3 M /au 2 . These hydrodynamical simulations are performed using FARGO-ADSG (Baruteau & Masset 2008;Baruteau 2008) over a polar mesh grid with N r = 395 and N s = 512 where N r and N s are the number of radial and azimuthal cells respectively.…”

Section: Gas Potentialmentioning

confidence: 99%

Modelling circumbinary protoplanetary disks

Lines

Leinhardt

Baruteau

et al. 2016

A&A

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Aims. We investigate the feasibility of planetesimal growth in circumbinary protoplanetary disks around the observed systems Kepler-16 and Kepler-34 under the gravitational influence of a precessing eccentric gas disk. Methods. We embed the results of our previous hydrodynamical simulations of protoplanetary disks around binaries into an N-body code to perform 3D, high-resolution, inter-particle gravity-enabled simulations of planetesimal growth and dynamics that include the gravitational force imparted by the gas. Results. Including the full, precessing asymmetric gas disk generates high eccentricity orbits for planetesimals orbiting at the edge of the circumbinary cavity, where the gas surface density and eccentricity have their largest values. The gas disk is able to efficiently align planetesimal pericenters in some regions leading to phased, non-interacting orbits. Outside of these areas eccentric planetesimal orbits become misaligned and overlap leading to crossing orbits and high relative velocities during planetesimal collisions. This can lead to an increase in the number of erosive collisions that far outweighs the number of collisions that result in growth. Gravitational focusing from the static axisymmetric gas disk is weak and does not significantly alter collision outcomes from the gas free case. Conclusions. Due to asymmetries in the gas disk, planetesimals are strongly perturbed onto highly eccentric orbits. Where planetesimals orbits are not well aligned, orbit crossings lead to an increase in the number of erosive collisions. This makes it difficult for sustained planetesimal accretion to occur at the location of Kepler-16b and Kepler-34b and we therefore rule out in situ growth. This adds further support to our initial suggestions that most circumbinary planets should form further out in the disk and migrate inwards.

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“…As such it is a surprise that the concept of a mmsn is still used in the consideration of initial conditions for planet forming discs (e.g. Simon et al 2015;Lines et al 2015;Bitsch et al 2015;Hopkins 2016;Coleman et al 2017;Mutter et al 2017) 3 . It is worth stressing that adoption of this could also be explained by FU Orionis type outburst cycles driven by e.g.…”

Section: Initial Conditions For Planet Formationmentioning

confidence: 99%

The Maximum Mass Solar Nebula and the early formation of planets

Nixon

King

Pringle

2018

Monthly Notices of the Royal Astronomical Society

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Current planet formation theories provide successful frameworks with which to interpret the array of new observational data in this field. However, each of the two main theories (core accretion, gravitational instability) is unable to explain some key aspects. In many planet formation calculations, it is usual to treat the initial properties of the planet forming disc (mass, radius, etc.) as free parameters. In this paper, we stress the importance of setting the formation of planet forming discs within the context of the formation of the central stars. By exploring the early stages of disc formation, we introduce the concept of the Maximum Mass Solar Nebula (MMSN), as opposed to the oft-used Minimum Mass Solar Nebula (here mmsn). It is evident that almost all protoplanetary discs start their evolution in a strongly self-gravitating state. In agreement with almost all previous work in this area, we conclude that on the scales relevant to planet formation these discs are not gravitationally unstable to gas fragmentation, but instead form strong, transient spiral arms. These spiral arms can act as efficient dust traps allowing the accumulation and subsequent fragmentation of the dust (but not the gas). This phase is likely to populate the disc with relatively large planetesimals on short timescales while the disc is still veiled by a dusty-gas envelope. Crucially, the early formation of large planetesimals overcomes the main barriers remaining within the core accretion model. A prediction of this picture is that essentially all observable protoplanetary discs are already planet hosting.

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Modelling circumbinary protoplanetary disks

Cited by 31 publications

References 36 publications

Circumbinary discs: Numerical and physical behaviour

Circumbinary discs: Numerical and physical behaviour

Modelling circumbinary protoplanetary disks

The Maximum Mass Solar Nebula and the early formation of planets

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