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The cosmological many-body problem is effectively an infinite system ofgravitationally interacting masses in an expanding universe. Despite theinteractions' long-range nature, an analytical theory of statistical mechanicsdescribes the spatial and velocity distribution functions which arise in thequasi-equilibrium conditions that apply to many cosmologies. Consequences ofthis theory agree well with the observed distribution of galaxies. Furtherconsequences such as thermodynamics provide insights into the physicalproperties of this system, including its robustness to mergers, and itstransition from a grand canonical ensemble to a collection of microcanonicalensembles with negative specific heat.

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