Application of three-body stability to globular clusters: II. Observed velocity dispersions

TL;DR

This study explains the velocity dispersion profiles in globular clusters without dark matter or MOND by applying three-body stability analysis, successfully predicting flattening in most clusters using orbital data.

Contribution

It introduces an analytical stability boundary for stars in GCs to predict velocity dispersion flattening, offering a Newtonian dynamics-based explanation.

Findings

Stability boundary predicts flattening in most clusters

Observational data align with stability boundary predictions

MOND not favored as the primary explanation in analyzed clusters

Abstract

The velocity dispersion profile in globular clusters (GCs) is explained here without having to rely on dark matter or a modification of Newtonian dynamics (MOND). The flattening of the velocity dispersion at large radii in certain Milky Way GCs, or lack thereof, is explained by recourse to the stability of the three-body problem in Newtonian dynamics. The previous paper in this series determined an analytical formula for the transition radius between stable and unstable orbits for a star in a GC. This stability boundary is used here to predict where the velocity dispersion profile is expected to flatten in GCs, given known orbital parameters of the GC-galaxy orbit. Published observational data for the velocity dispersion as a function of radius of 15 Milky Way GCs with approximately known orbital parameters are used here. We find that the stability boundary predicts flattening in the majority of clusters. While observational uncertainties in the orbital parameters prevent MOND from being ruled out entirely for some clusters, it is not the preferred model in any cluster. Based on the results of this study, we recommend further velocity dispersion observations and orbital determination for NGC 6171 and NGC 6341 as these are promising candidates for distinguishing Newtonian and MOND models. In particular, NGC 6171 may already be showing evidence of the chaotic diffusion of stars leading to flattening at the predicted stability boundary.