2008
DOI: 10.1063/1.2839124
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Infinite self-gravitating systems and cosmological structure formation

Abstract: The usual thermodynamic limit for systems of classical self-gravitating point particles becomes well defined, as a {\it dynamical} problem, using a simple physical prescription for the calculation of the force, equivalent to the so-called ``Jeans' swindle''. The relation of the resulting intrinsically out of equilibrium problem, of particles evolving from prescribed uniform initial conditions in an infinite space, to the one studied in current cosmological models (in an expanding universe) is explained. We the… Show more

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Cited by 10 publications
(15 citation statements)
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“…[10]). Nevertheless, several recent works [38,36,30,26,31] vindicate its validity using a variety of arguments, and we would like to claim that the reasoning above supports their main conclusions. In particular, we claim that the law of gravity should be such that an infinite fluid with constant density is an (unstable) static equilibrium solution, where the net force felt by every point, averaged over such a homogeneous and isotropic background, vanishes.…”
Section: Numerical Simulationssupporting
confidence: 51%
See 1 more Smart Citation
“…[10]). Nevertheless, several recent works [38,36,30,26,31] vindicate its validity using a variety of arguments, and we would like to claim that the reasoning above supports their main conclusions. In particular, we claim that the law of gravity should be such that an infinite fluid with constant density is an (unstable) static equilibrium solution, where the net force felt by every point, averaged over such a homogeneous and isotropic background, vanishes.…”
Section: Numerical Simulationssupporting
confidence: 51%
“…[10]). Nevertheless, several recent works [38,36,30,26,31] vindicate its validity using a variety of arguments, and we would like to claim that the reasoning above supports their main conclusions. In particular, we 3 Otherwise, it is easy to verify that a solution of the form ρ(r, t) = ρ0 a(t) can be found, where the cosmic scale factor a(t) is exactly the same as in a fully relativistic Lematre-Friedmann-Robertson-Walker universe.…”
Section: Numerical Simulationsmentioning
confidence: 52%
“…Since we are interested in a phenomenon related to the discreteness of particles, the thermodynamic limit is taken here. For a discussion of the two limits see reference [12].…”
Section: Chymentioning
confidence: 99%
“…In the SL limit, the local equilibrium in S a is entirely determined by the local packing fraction η a (r) = ηρ a (r)/ρ. In particular, the decay of particle correlations is controlled by the local hard-sphere correlation length [15,16] λ a (r) = σ a ξ HS (η a (r)) (34) where ξ HS (η) is some dimensionless function of η. Let us assume a priori that the system remains in a fluid phase at the local level, i.e.…”
Section: Separation Of Scales and The Hydrostatic Balancementioning
confidence: 99%
“…For the description of the Universe, the introduction of a box seems a necessity for any thermodynamical theory in the absence of cosmological expansion[34].…”
mentioning
confidence: 99%