A Universal Formation Mechanism for Open and Globular Clusters in Turbulent Gas

TLDR

Cluster structural differences arise from variations in formation pressure and subsequent age evolution. A universal formation mechanism, driven by turbulent gas, explains the mass distribution and evolutionary differences of globular, open, and unbound clusters, with an initial n(M)∝M⁻², age‑dependent mass loss, and a luminosity peak governed solely by age rather than host galaxy luminosity.

Abstract

A universal mechanism for cluster formation in all epochs and environments is found to be consistent with the properties and locations of young and old globular clusters, open clusters and unbound associations, and interstellar clouds. The primary structural differences between various cluster types result from differences in pressure at the time of formation, combined with different ages for subsequent evolution. All clusters begin with a mass distribution similar to that for interstellar clouds, which is approximately n(M)dM ∝ M-2 dM. Old halo globulars have a current mass distribution that falls off at low mass because of a Hubble time of cluster destruction. Young globulars have not yet had time for a similar loss, and some old open clusters have survived because of their low densities. The peak in the halo cluster luminosity function depends only on age, and is independent of the host galaxy luminosity, as observed. The peak globular cluster mass is not a characteristic or Jeans mass in the primordial galaxy, as previously suggested.