On the possible critical behaviour of a marginally stable stellar disc

TL;DR

This paper models marginally stable stellar discs as systems near a phase transition, revealing critical phenomena and potential spontaneous spiral structure formation through hydrodynamic analysis and numerical simulations.

Contribution

It introduces a thermodynamic analogy to stellar disc stability, identifying a critical point analogous to a gas-liquid transition and analyzing associated critical exponents.

Findings

Power-law scaling of the order parameter near the critical point

Identification of spiral structure formation as a phase transition outcome

Numerical evidence of stellar splinters and crescents as critical phenomena

Abstract

Using hydrodynamic approach, it is shown that the properties of a marginally stable collisionless stellar disc resemble those of a thermodynamic system undergoing a gas--liquid phase transition. The maximum in Toomre's stability diagram, which separates gravitationally stable and unstable states with respect to axisymmetric perturbations, can be treated as a critical point for this transition. Static perturbations of stellar density are explored and the mean perturbation amplitude is considered as the order parameter of the theory. The disc's state is assumed to change as the disc passes through the critical point. Since the disc tends to retain hydrostatic equilibrium, structures can be formed spontaneously, identifiable with a seed spiral structure. A power-law scaling of the order parameter in the vicinity of the critical point has been found. The susceptibility and other Landau--Weiss exponents similar to those in the Van der Waals theory are calculated. The critical behaviour of marginally stable discs at the initial stage of their evolution occurs in numerical simulations where snapshots of stellar positions reveal stellar splinters and crescents diverging from the disc centre. These structures can be a result of the phase transition. In numerical simulations, these structures eventually reduce to decaying worm-type features because of the `heating' most likely resulting from instability of stellar orbits due to resonances. Under favourable conditions the critical behaviour leading to the establishment of order in a stellar disc can result in the generation of a spiral structure.