Nonlinear outcome of gravitational instability in an irradiated protoplanetary disc

Abstract

Using local three dimensional radiation hydrodynamics simulations, the nonlinear outcome of gravitational instability in an irradiated protoplanetary disc is investigated in a parameter space of the surface density $\Sigma$ and the radius $r$. Starting from laminar flow, axisymmetric self-gravitating density waves grow first. Their self-gravitating degree becomes larger when $\Sigma$ is larger or the cooling time is shorter at larger radii. The density waves eventually collapse owing to non-axisymmetric instability, which results in either fragmentation or gravito-turbulence after a transient phase. The boundaries between the two are found at $r\sim 75$ AU as well as at the $\Sigma$ that corresponds to the initial Toomre's parameter of $\sim 0.2$. The former boundary corresponds to the radius where the cooling time becomes short, approximating unity. Even when gravito-turbulence is established around the boundary radius, such a short cooling time inevitably makes the fluctuation of $\Sigma$ large enough to trigger fragmentation. On the other hand, when $\Sigma$ is beyond the latter boundary (i.e. the initial Toomre's parameter is less than $\sim 0.2$), the initial laminar flow is so unstable against self-gravity that it evolves into fragmentation regardless of the radius or, equivalently, the cooling time. Runaway collapse follows fragmentation when the mass concentration at the centre of a bound object is high enough that the temperature exceeds the H${}_2$ dissociation temperature.

arXiv commentaccepted for publication in MNRAS

References in corpus (39)

• Spectral Energy Distributions of T Tauri Stars With Passive Circumstellar Disks
• Low Temperature Opacities
• Nonlinear Outcome of Gravitational Instability in Cooling, Gaseous Disks
• The Mass Dependence Between Protoplanetary Disks and their Stellar Hosts
• Rosseland and Planck Mean Opacities for Protoplanetary Discs
• Gravitational Instabilities in Circumstellar Disks
• Can giant planets form by direct gravitational instability?
• Investigating fragmentation conditions in self-gravitating accretion discs
• Spiral Density Waves in a Young Protoplanetary Disk
• Challenges in Forming Planets by Gravitational Instability: Disk Irradiation and Clump Migration, Accretion & Tidal Destructio
• Radiation Magnetohydrodynamic Simulations of Protostellar Collapse: Protostellar Core Formation
• Pseudo-viscous modeling of self-gravitating discs and the formation of low mass ratio binaries
• Vertical Structure of Gas Pressure-Dominated Accretion Disks with Local Dissipation of Turbulence and Radiative Transport
• Characterising the Gravitational Instability in Cooling Accretion Discs
• A Module for Radiation Hydrodynamic Calculations With ZEUS-2D Using Flux-Limited Diffusion
• Nonlinear Outcome of Gravitational Instability in Disks with Realistic Cooling
• Implementation of the Shearing Box Approximation in Athena
• On the convergence of the critical cooling timescale for the fragmentation of self-gravitating discs
• Non-convergence of the critical cooling timescale for fragmentation of self-gravitating discs
• Time-dependent models of the structure and evolution of self-gravitating protoplanetary discs
• The Mass Budget of Planet Forming Discs: Isolating the Epoch of Planetesimal Formation
• Numerical convergence in self-gravitating shearing sheet simulations and the stochastic nature of disc fragmentation
• The role of thermodynamics in disc fragmentation
• Stability of self-gravitating discs under irradiation
• Resolution requirements for Smoothed Particle Hydrodynamics simulations of self-gravitating accretion discs
• Effects of radiation transfer on the structure of self-gravitating disks, their fragmentation and evolution of the fragments
• A revised condition for self-gravitational fragmentation of protoplanetary disks
• Turbulent Disks are Never Stable: Fragmentation and Turbulence-Promoted Planet Formation
• Gas Properties and Implications for Galactic Star Formation in Numerical Models of the Turbulent, Multiphase ISM
• Resolved images of self-gravitating circumstellar discs with ALMA
• Gravito-Turbulent Disks in 3D: Turbulent Velocities vs. Depth
• The fragmentation of protostellar discs: the Hill criterion for spiral arms
• Magnetic Turbulence and Thermodynamics in the Inner Region of Protoplanetary Discs
• On the gravitational stability of gravito-turbulent accretion disks
• The Effect of Irradiation on the Jeans Mass in Fragmenting Self-Gravitating Protostellar Discs
• The Effect of Protoplanetary Disk Cooling Times on the Formation of Gas Giant Planets by Gravitational Instability
• The Role of the Cooling Prescription for Disk Fragmentation: Numerical Convergence & Critical Cooling Parameter in Self-Gravitating Disks
• Gravito-turbulence in irradiated protoplanetary discs
• Gravitoturbulence in magnetised protostellar discs

Cited by in corpus (7)

• 3D Radiation Hydrodynamic Simulations of Gravitational Instability in AGN Accretion Disks: Effects of Radiation Pressure
• Spiral structures in gravito-turbulent gaseous disks
• Magnetohydrodynamics in a Cylindrical Shearing Box
• Optab: Public code for generating gas opacity tables for radiation hydrodynamics simulations
• Gravito-turbulence in local disk simulations with an adaptive moving mesh
• Standing solitary waves as transitions to spiral structures in gravitationally unstable accretion disks
• Nonlinear analysis of gravitational instability in a 3D gaseous disc