Orbital Instabilities in a Triaxial Cusp Potential

TL;DR

This paper presents an analytic triaxial potential model for astrophysical systems, demonstrating a robust orbit instability that impacts dark matter halos, galactic bulges, and star clusters, with implications for their formation and evolution.

Contribution

It introduces a new analytic form of a triaxial potential based on a specific density profile, revealing orbit instabilities in such systems and providing insights into their astrophysical dynamics.

Findings

Orbit instability exists in triaxial systems with this potential.

Unstable orbits can grow and saturate, affecting system evolution.

Analytic models clarify the physics behind the instability.

Abstract

This paper constructs an analytic form for a triaxial potential that describes the dynamics of a wide variety of astrophysical systems, including the inner portions of dark matter halos, the central regions of galactic bulges, and young embedded star clusters. Specifically, this potential results from a density profile of the form $\rho (m) \propto m^{-1}$, where the radial coordinate is generalized to triaxial form so that $m^2 = x^2/a^2 + y^2/b^2 + z^2/c^2 $. Using the resulting analytic form of the potential, and the corresponding force laws, we construct orbit solutions and show that a robust orbit instability exists in these systems. For orbits initially confined to any of the three principal planes, the motion in the perpendicular direction can be unstable. We discuss the range of parameter space for which these orbits are unstable, find the growth rates and saturation levels of the instability, and develop a set of analytic model equations that elucidate the essential physics of the instability mechanism. This orbit instability has a large number of astrophysical implications and applications, including understanding the formation of dark matter halos, the structure of galactic bulges, the survival of tidal streams, and the early evolution of embedded star clusters.