Remarks about the thermodynamic limit in selfgravitating systems

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dc.creatorVelazquez, L.
dc.creatorGuzman, F.
dc.date2003-09-15
dc.date.accessioned2026-07-07T02:09:34Z
dc.date.available2026-07-07T02:09:34Z
dc.descriptionThe present effort addresses the question about the existence of a well-defined thermodynamic limit for the astrophysical systems with the following power law form: to tend the number of particles, N, the total energy, E, and the characteristic linear dimension of the system, L, to infinity, keeping constant E/N^{Λ_{E}} and L/N^{Λ_{L}}, being Λ_{E} and Λ_{L} certain scaling exponent constant. This study is carried out for a system constituted by a non-rotating fluid under the influence of its own Newtonian gravitational interaction. The analysis yields that a thermodynamic limit of the above form will only appear when the local pressure depends on the energy density of fluid as $p=γε$, being $γ$ certain constant. Therefore, a thermodynamic limit with a power law form can be only satisfied by a reduced set of models, such as the selfgravitating gas of fermions and the Antonov isothermal model.
dc.descriptionRevTex 4, 4 pages. Comments about the de Vega and Sanchez discussion with V. Laliena about the applicability of the diluted limit in selfgravitating systems
dc.identifierhttps://arxiv.org/abs/astro-ph/0309386
dc.identifierhttp://arxiv.org/abs/astro-ph/0309386
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/6480
dc.subjectAstrophysics
dc.titleRemarks about the thermodynamic limit in selfgravitating systems
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