Equilibrium Initialization and Stability of Three-Dimensional Gas Disks

TL;DR

This paper introduces a new systematic method for setting up stable three-dimensional galactic gas disks based on hydrodynamic equilibrium, and investigates their stability and spiral formation through simulations.

Contribution

It presents two novel approaches, the density and potential methods, for initializing stable gas disks in equilibrium for detailed stability analysis.

Findings

Threshold for disk instability is reduced in thick disks.

Self-induced spirals match theoretical predictions.

Thick disks are more stable against gravitational collapse.

Abstract

We present a new systematic way of setting up galactic gas disks based on the assumption of detailed hydrodynamic equilibrium. To do this, we need to specify the density distribution and the velocity field which supports the disk. We first show that the required circular velocity has no dependence on the height above or below the midplane so long as the gas pressure is a function of density only. The assumption of disks being very thin enables us to decouple the vertical structure from the radial direction. Based on that, the equation of hydrostatic equilibrium together with the reduced Poisson equation leads to two sets of second-order non-linear differential equation, which are easily integrated to set-up a stable disk. We call one approach `density method' and the other one `potential method'. Gas disks in detailed balance are especially suitable for investigating the onset of the gravitational instability. We revisit the question of global, axisymmetric instability using fully three-dimensional disk simulations. The impact of disk thickness on the disk instability and the formation of spontaneously induced spirals is studied systematically with or without the presence of the stellar potential. In our models, the numerical results show that the threshold value for disk instability is shifted from unity to 0.69 for self-gravitating thick disks and to 0.75 for combined stellar and gas thick disks. The simulations also show that self-induced spirals occur in the correct regions and with the right numbers as predicted by the analytic theory.