Ensemble in-equivalence in supernova matter within a simple model
arXiv:1110.2034 · doi:10.1103/PhysRevC.85.025803
Abstract
A simple, exactly solvable statistical model is presented for the description of baryonic matter in the thermodynamic conditions associated to the evolution of core-collapsing supernova. It is shown that the model presents a first order phase transition in the grandcanonical ensemble which is not observed in the canonical ensemble. Similar to other model systems studied in condensed matter physics, this ensemble in-equivalence is accompanied by negative susceptibility and discontinuities in the intensive observables conjugated to the order parameter. This peculiar behavior originates from the fact that baryonic matter is subject to attractive short range strong forces as well as repulsive long range electromagnetic interactions, partially screened by a background of electrons. As such, it is expected in any theoretical treatment of nuclear matter in the stellar environment. Consequences for the phenomenology of supernova dynamics are drawn.
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Cited by in corpus (13)
- Unified treatment of sub-saturation stellar matter at zero and finite temperature
- A new temperature dependent hyperonic equation of state: application to rotating neutron star models and I-Q-relations
- Heavy Baryons in Compact Stars
- Densities and energies of nuclei in dilute matter
- Clusterized nuclear matter in the (proto-)neutron star crust and the symmetry energy
- Light clusters in dilute heavy-baryon admixed nuclear matter
- Inhomogeneous condensates in dilute nuclear matter and BCS-BEC crossovers
- Hyperonization in compact stars
- Phase diagram of neutron-rich nuclear matter and its impact on astrophysics
- Transformation between statistical ensembles in the modelling of nuclear fragmentation
- Selected problems in astrophysics of compact objects
- Some aspects of the phase diagram of nuclear matter relevant to compact stars
- Neutron-rich nuclei and the equation of state of stellar matter