Equilibrium Sequences and Gravitational Instability of Rotating Isothermal Rings

TL;DR

This study models rotating isothermal rings in galaxies to analyze their gravitational stability, revealing how parameters like thermal energy and rotation influence their propensity to become unstable and form stars.

Contribution

It introduces a self-consistent method to construct equilibrium sequences of rotating isothermal rings and examines their stability, highlighting the effects of thermal energy and rotation.

Findings

Smaller alpha rings are more unstable with broader azimuthal mode ranges.

Rotation suppresses instability when angular frequency exceeds a critical value.

Observed star-forming rings without azimuthal age gradients are gravitationally unstable.

Abstract

Nuclear rings at centers of barred galaxies exhibit strong star formation activities. They are thought to undergo gravitational instability when sufficiently massive. We approximate them as rigidly-rotating isothermal objects and investigate their gravitational instability. Using a self-consistent field method, we first construct their equilibrium sequences specified by two parameters: alpha corresponding to the thermal energy relative to gravitational potential energy, and R_B measuring the ellipticity or ring thickness. Unlike in the incompressible case, not all values of R_B yield an isothermal equilibrium, and the range of R_B for such equilibria shrinks with decreasing alpha. The density distributions in the meridional plane are steeper for smaller alpha, and well approximated by those of infinite cylinders for slender rings. We also calculate the dispersion relations of nonaxisymmetric modes in rigidly-rotating slender rings with angular frequency Omega_0 and central density rho_max. Rings with smaller alpha are found more unstable with a larger unstable range of the azimuthal mode number. The instability is completely suppressed by rotation when Omega_0 exceeds the critical value. The critical angular frequency is found to be almost constant at ~ 0.7 sqrt(G*rho_c) for alpha > 0.01 and increases rapidly for smaller alpha. We apply our results to a sample of observed star-forming rings and confirm that rings without a noticeable azimuthal age gradient of young star clusters are indeed gravitationally unstable.