2001/01/31 by H. J. de Vega, H.J. de Vega, N. Sánchez +1 · 3 citations
Engineering · Physics and Astronomy · #Canonical ensemble #Critical point (mathematics) #Fluid dynamics and aerodynamics studies #Fractal #Hydrostatic equilibrium #Ideal gas #Monte Carlo method #Saddle point #Statistical Mechanics and Entropy #Statistical mechanics #Theoretical and Computational Physics #Thermodynamic equilibrium #Thermodynamic limit #astro-ph #cond-mat #gr-qc #hep-th
paper · pdf · doi:10.1016/s0550-3213(02)00026-3
published as Nucl.Phys. B625 (2002) 460-494 · Latex, 37 pages, 12 .ps figures, to appear in Nucl. Phys. B
arxiv created 2002/01/31 · openalex publication_date 2002/03/01 · arxiv updated 2009/11/30 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We complete our study of the selfgravitating gas by computing the fluctuations around the saddle point solution for the three statistical ensembles. Although the saddle point is the same for the three ensembles, the fluctuations change from one ensemble to another. The zeroes of the fluctuations determinant determine the position of the critical points for each ensemble.This yields the domains of validity of the mean field approach. Only the S wave determinant exhibits critical points.Closed formulae for the S and P wave determinants are derived.The local properties of the selfgravitating gas in thermodynamic equilibrium are studied in detail. The pressure, energy density, particle density and speed of sound are computed and analyzed as functions of the position. The equation of state turns out to be locally p(r) = T rho(r) as for the ideal gas. Starting from the partition function of the selfgravitating gas, we prove in this microscopic calculation that the hydrostatic description yielding locally the ideal gas equation of state is exact in the N = infinity limit. The dilute nature of the thermodynamic limit(N, L -> infinity with N/L fixed) together with the long range nature of the gravitational forces play a crucial role in the obtention of such ideal gas equation. The self-gravitating gas being inhomogeneous, we have PV/[NT] = f(eta) leq 1 for any finite volume V. The inhomogeneous particle distribution in the ground state suggests a fractal distribution with Haussdorf dimension D, D is slowly decreasing with increasing density, 1 lesssim D < 3. The average distance between particles is computed in Monte Carlo simulations andanalytically in the mean field approach. A dramatic drop at the phase transition is exhibited, clearly illustrating the properties of the collapse.