A New Thermodynamics, From Nuclei to Stars

Details A New Thermodynamics, From Nuclei to Stars A New Thermodynamics, From Nuclei to Stars

2003-02-13

arxiv.org/abs/cond-mat/0302267v2

Physics

Condensed Matter

Statistical Mechanics

17 pages, 7 figures, Latex file, presented at XLI International Winter Meeting on Nuclear Physics, Bormio, It. Figure captions

Scientific paper

Equilibrium statistics of Hamiltonian systems is correctly described by the microcanonical ensemble. Classically this is the manifold of all points in the $N-$body phase space with the given total energy. Due to Boltzmann's principle, $e^S=tr(\delta(E-H))$, its geometrical size is related to the entropy $S(E,N,...)$. This definition does not invoke any information theory, no thermodynamic limit, no extensivity, and no homogeneity assumption, as are needed in conventional (canonical) thermo-statistics. Therefore, it describes the equilibrium statistics of extensive as well of non-extensive systems. Due to this fact it is the {\em fundamental} definition of any classical equilibrium statistics. It can address nuclei and astrophysical objects as well. All kind of phase transitions can be distinguished sharply and uniquely for even small systems. For transitions in nuclear physics the scaling to an hypothetical uncharged nuclear matter with an $N/Z-$ ratio like realistic nuclei is not needed.

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