The Effect of Spacetime Curvature on Statistical Distributions

TL;DR

This paper derives the equilibrium distribution function for particles in curved spacetime, showing how spacetime curvature influences physical observables and distribution shapes, extending classical statistical mechanics into relativistic regimes.

Contribution

It introduces a framework for deriving thermodynamic equilibrium distributions in curved spacetime, accounting for general relativity effects on statistical ensembles.

Findings

Spacetime curvature modifies the shape of the distribution function.

Relativistic effects can lead to decreasing density and increasing azimuthal velocity.

Kinetic energy in Kerr-Newman spacetime approaches classical equipartition at large radii.

Abstract

The Boltzmann distribution of an ideal gas is determined by the Hamiltonian function generating single particle dynamics. Systems with higher complexity often exhibit topological constraints, which are independent of the Hamiltonian and may affect the shape of the distribution function as well. Here, we study a further source of heterogeneity, the curvature of spacetime arising from the general theory of relativity. The present construction relies on three assumptions: first, the statistical ensemble is made of particles obeying geodesic equations, which define the phase space of the system. Next, the metric coefficients are time-symmetric, implying that, if thermodynamic equilibrium is achieved, all physical observables are independent of coordinate time. Finally, ergodicity is enforced with respect to proper time, so that ambiguity in the choice of a time variable for the statistical ensemble is removed. Under these hypothesis, we derive the distribution function of thermodynamic equilibrium, and verify that it reduces to the Boltzmann distribution in the classical limit. We further show that spacetime curvature affects physical observables, even far from the source of the metric. Two examples are analyzed: an ideal gas in Schwarzschild spacetime and a charged gas in Kerr-Newman spacetime. In the Schwarzschild case, conservation of macroscopic constraints, such as angular momentum, combined with relativistic distortion of the distribution function can produce configurations with decreasing density and growing azimuthal rotation velocity far from the event horizon of the central mass. In the Kerr-Newman case, it is found that kinetic energy associated with azimuthal rotations is an increasing function of the radial coordinate, and it eventually approaches a constant value corresponding to classical equipartition, even though spatial particle density decreases.