Treating gravity in thin disk simulations

TL;DR

This paper develops a method to accurately determine the gravitational potential smoothing length in 2D thin disk simulations, ensuring realistic force calculations and improving the modeling of planet-disk interactions and disk fragmentation.

Contribution

It provides a systematic way to evaluate the smoothing length in 2D simulations based on vertical disk structure, aligning 2D results more closely with 3D physics.

Findings

For large distances, smoothing length b5bequal to 0.7H for planets and 1.2H for self-gravity.

Proper smoothing affects disk fragmentation and migration direction.

The method offers a fast approximation matching full 3D simulation results.

Abstract

In 2D simulations of thin gaseous disks with embedded planets or self-gravity the gravitational potential needs to be smoothed to avoid singularities in the numerical evaluation of the gravitational potential or force. In order to correctly resemble the realistic case of vertically extended 3D disks the softening prescription used in 2D needs to be adjusted properly. In this paper we analyze the embedded planet and the self-gravity case and provide a method to evaluate the required smoothing in 2D simulations of thin disks. Starting from the averaged hydrodynamic equations and using a vertically isothermal disk model, we calculate the force. We compare our results to the often used Plummer form of the potential which runs as \propto 1/(r^2+\epsilon^2)^{1/2}. For that purpose we compute the required smoothing length \epsilon as a function of distance r to the planet or to a disk element within a self-gravitating disk. We find that for larger distances \epsilon is determined solely by the vertical disk thickness H. For the planet case we find that outside r\simH a value of \epsilon = 0.7H describes the averaged force very well, while in the self-gravitating disk the value needs to be larger, \epsilon = 1.2H. For smaller distances the smoothing needs to be reduced significantly. Comparing torque densities of 3D and 2D simulations we show that the modification to the vertical density stratification as induced by an embedded planet needs to be taken into account to obtain agreeing results. In disk fragmentation simulations the choice of \epsilon can determine whether a disk will fragment or not. Because a wrong smoothing length can change even the direction of migration, it is very important to include the effect of the planet on the local scale height in 2D planet-disk simulations. We provide an approximate and fast method for this purpose which gives very good agreement to full 3D simulations.