Ising Analogue to Compact-Star Matter

Napolitani, P.; Chomaz, Ph.; Gulminelli, F.; Hasnaoui, Karim

doi:10.1103/physrevlett.98.131102

Cited by 22 publications

(31 citation statements)

References 28 publications

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“…Because of the very high electron incompressibility, the convexity observed in the baryonic part of the energy density is not present any more in the total thermodynamic potential. This is known in the literature as the quenching of the phase transition due to Coulomb frustration [84,85], and shows [86] that convexities in the (free) energy density do not necessarily correspond to instabilities in the physical system. This shows that if one wants to formulate the equilibrium problem in the grandcanonical ensemble, one has to account for the electron zero point motion.…”

Section: E Phase Transitions In the Inner Crust?mentioning

confidence: 99%

Unified treatment of subsaturation stellar matter at zero and finite temperature

2015

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33 pages, 15 figures; submitted to Phys. Rev. CInternational audienceThe standard variational derivation of stellar matter structure in the Wigner-Seitz approximation is generalized to the finite temperature situation where a wide distribution of different nuclear species can coexist in the same density and proton fraction condition, possibly out of $\beta$-equilibrium. The same theoretical formalism is shown to describe on one side the single-nucleus approximation (SNA), currently used in most core collapse supernova simulations, and on the other side the nuclear statistical equilibrium (NSE) approach, routinely employed in r- and p-process explosive nucleosynthesis problems. In particular we show that in-medium effects have to be accounted for in NSE to have a theoretical consistency between the zero and finite temperature modeling. The bulk part of these in-medium effects is analytically calculated and shown to be different from a van der Waals excluded volume term. This unified formalism allows controlling quantitatively the deviations from the SNA in the different thermodynamic conditions, as well as having a NSE model which is reliable at any arbitrarily low value of the temperature, with potential applications for neutron star cooling and accretion problems. We present different illustrative results with several mass models and effective interactions, showing the importance of accounting for the nuclear species distribution even at temperatures lower than 1 MeV

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Section: E Phase Transitions In the Inner Crust?mentioning

confidence: 99%

Unified treatment of subsaturation stellar matter at zero and finite temperature

2015

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“…In the crust of a neutron star the transition from the Wigner crystal phase to the quantum liquid also proceeds through a cluster phase as a function of density [8]. Clustering occurs as a transition between the quantum liquid and solid state phases because of frustration effects, that is, due to the interplay between an attractive and a repulsive interac-tion [9,10]. This is the case in the crust of neutron stars or for gelification in condensed matter.…”

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confidence: 99%

Cluster-liquid transition in finite, saturated fermionic systems

et al. 2014

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“…It has been argued in ref. [16] that this generic frustration effect should lead to a quenching of the first order phase transition. We have shown that the phase transition is observed in the grandcanonical ensemble.…”

Section: Grandcanonical Formulationmentioning

confidence: 96%

Ensemble inequivalence in supernova matter within a simple model

Gulminelli

Raduta²

2012

Phys. Rev. C

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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 environement. Consequences for the phenomenology of supernova dynamics are drawn.

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Ising Analogue to Compact-Star Matter

Cited by 22 publications

References 28 publications

Unified treatment of subsaturation stellar matter at zero and finite temperature

Unified treatment of subsaturation stellar matter at zero and finite temperature

Cluster-liquid transition in finite, saturated fermionic systems

Ensemble inequivalence in supernova matter within a simple model

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