Numerical convergence in self-gravitating disc simulations: initial conditions and edge effects

Details Numerical convergence in self-gravitating disc simulations: initial conditions and edge effects Numerical convergence in self-gravitating disc simulations: initial conditions and edge effects

2011-06-22

arxiv.org/abs/1106.4425v1

Astronomy and Astrophysics

Astrophysics

Earth and Planetary Astrophysics

5 pages, 5 figures, accepted for publication in MNRAS

Scientific paper

We study the numerical convergence of hydrodynamical simulations of self-gravitating accretion discs, in which a simple cooling law is balanced by shock heating. It is well-known that there exists a critical cooling time scale for which shock heating can no longer compensate for the energy losses, at which point the disc fragments. The numerical convergence of previous results of this critical cooling time scale was questioned recently using Smoothed Particle Hydrodynamics (SPH). We employ a two-dimensional grid-based code to study this problem, and find that for smooth initial conditions, fragmentation is possible for slower cooling as the resolution is increased, in agreement with recent SPH results. We show that this non-convergence is at least partly due to the creation of a special location in the disc, the boundary between the turbulent and the laminar region, when cooling towards a gravito-turbulent state. Converged results appear to be obtained in setups where no such sharp edges appear, and we then find a critical cooling time scale of ~ 4 $\Omega^{-1}$, where $\Omega$ is the local angular velocity.

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