Statistical Mechanics of the Cosmological Many-body Problem and its Relation to Galaxy Clustering

TL;DR

This paper develops a statistical mechanics framework for the cosmological many-body problem, explaining galaxy clustering and system properties in an expanding universe with long-range gravitational interactions.

Contribution

It introduces an analytical statistical mechanics theory for gravitationally interacting masses in cosmology, linking it to observed galaxy distributions and thermodynamic properties.

Findings

Theory matches observed galaxy distributions

Insights into system robustness and phase transitions

Description of thermodynamic behavior in cosmological context

Abstract

The cosmological many-body problem is effectively an infinite system of gravitationally interacting masses in an expanding universe. Despite the interactions' long-range nature, an analytical theory of statistical mechanics describes the spatial and velocity distribution functions which arise in the quasi-equilibrium conditions that apply to many cosmologies. Consequences of this theory agree well with the observed distribution of galaxies. Further consequences such as thermodynamics provide insights into the physical properties of this system, including its robustness to mergers, and its transition from a grand canonical ensemble to a collection of microcanonical ensembles with negative specific heat.