Critical temperature for the nuclear liquid-gas phase transition (from multifragmentation and fission)

Karnaukhov, V.A.; Oeschler, H.; Budzanowski, A.; Avdeyev, S. P.; Botvina, A. S.; Cherepanov, E. A.; Karcz, W.; Kirakosyan, V. V.; Rukoyatkin, P.; Skwirczyńska, I.; Norbeck, E.

doi:10.1134/s1063778808120077

Cited by 33 publications

(43 citation statements)

References 36 publications

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“…11), which a realistic equation of state mus equation of state is in agreement with all the For comparison the acceptable radius interva Ref. [37] is also shown. Figure 12 shows a typical calculated densi neutron star with mass M = 1.97 M using G ⇢ (i.e.…”

Section: Constraints From Neutron Starssupporting

confidence: 63%

“…The only empirically founded phase transition discussed in this region is the one from a nuclear Fermi liquid to an interacting gas of nucleons [34,35,36,37,38].…”

Section: Notes On Thermodynamics and Dense Baryonic Mattermentioning

confidence: 99%

“…Mass radius relation for neutron star matter. The massradius constraints from reference [3], the radius constraint [37] and the two-solar-mass neutron stars [1,2] are shown for comparison.…”

Section: Constraints From Neutron Starsmentioning

confidence: 99%

“…(131). We recall that the critical temperature deduced from various nuclear reactions and multifragmentation experiments is T c = 17.9 ± 0.4 MeV [37,38].…”

Section: Nuclear Thermodynamics and The Liquid-gas Transitionmentioning

confidence: 99%

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Functional renormalization group studies of nuclear and neutron matter

Drews

Weise

2017

Progress in Particle and Nuclear Physics

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Functional renormalization group (FRG) methods applied to calculations of isospinsymmetric and asymmetric nuclear matter as well as neutron matter are reviewed. The approach is based on a chiral Lagrangian expressed in terms of nucleon and meson degrees of freedom as appropriate for the hadronic phase of QCD with spontaneously broken chiral symmetry. Fluctuations beyond mean-field approximation are treated solving Wetterich's FRG flow equations. Nuclear thermodynamics and the nuclear liquid-gas phase transition are investigated in detail, both in symmetric matter and as a function of the proton fraction in asymmetric matter. The equations of state at zero temperature of symmetric nuclear matter and pure neutron matter are found to be in good agreement with advanced ab-initio many-body computations. Contacts with perturbative many-body approaches (in-medium chiral perturbation theory) are discussed. As an interesting test case, the density dependence of the pion mass in the medium is investigated. The question of chiral symmetry restoration in nuclear and neutron matter is addressed. A stabilization of the phase with spontaneously broken chiral symmetry is found to persist up to high baryon densities once fluctuations beyond mean-field are included. Neutron star matter including beta equilibrium is discussed under the aspect of the constraints imposed by the existence of two-solar-mass neutron stars.

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Section: Constraints From Neutron Starssupporting

confidence: 63%

“…The only empirically founded phase transition discussed in this region is the one from a nuclear Fermi liquid to an interacting gas of nucleons [34,35,36,37,38].…”

Section: Notes On Thermodynamics and Dense Baryonic Mattermentioning

confidence: 99%

Section: Constraints From Neutron Starsmentioning

confidence: 99%

“…(131). We recall that the critical temperature deduced from various nuclear reactions and multifragmentation experiments is T c = 17.9 ± 0.4 MeV [37,38].…”

Section: Nuclear Thermodynamics and The Liquid-gas Transitionmentioning

confidence: 99%

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Functional renormalization group studies of nuclear and neutron matter

Drews

Weise

2017

Progress in Particle and Nuclear Physics

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“…This is remarkable, given the very different approaches. Whereas the temperature of the critical point is 15.1 MeV in χEFT, it is shifted to a value of T c = 18.3 MeV in the RG treatment of the nucleon-meson model, in good agreement with empirical results [16]. In order to address the entanglement between chemical freeze-out points and chiral restoration, the chiral condensate is studied as a function of temperature and chemical potential.…”

Section: Resultssupporting

confidence: 64%

Dense nucleonic matter and the renormalization group

Drews

Hell

Klein

et al. 2014

EPJ Web of Conferences

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Abstract. Fluctuations are included in a chiral nucleon-meson model within the framework of the functional renormalization group. The model, with parameters fitted to reproduce the nuclear liquid-gas phase transition, is used to study the phase diagram of QCD. We find good agreement with results from chiral effective field theory. Moreover, the results show a separation of the chemical freeze-out line and chiral symmetry restoration at large baryon chemical potentials.

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Nuclear Equation of State for Compact Stars and Supernovae

Burgio

Fantina

2018

Astrophysics and Space Science Library

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The equation of state (EoS) of hot and dense matter is a fundamental input to describe static and dynamical properties of neutron stars, core-collapse supernovae and binary compact-star mergers. We review the current status of the EoS for compact objects, that have been studied with both ab-initio many-body approaches and phenomenological models. We limit ourselves to the description of EoSs with purely nucleonic degrees of freedom, disregarding the appearance of strange baryonic matter and/or quark matter. We compare the theoretical predictions with different data coming from both nuclear physics experiments and astrophysical observations. Combining the complementary information thus obtained greatly enriches our insight into the dense nuclear matter properties. Current challenges in the description of the EoS are also discussed, mainly focusing on the model dependence of the constraints extracted from either experimental or observational data, the lack of a consistent and rigorous many-body treatment at zero and finite temperature of the matter encountered in compact stars (e.g. problem of cluster formation and extension of the EoS to very high temperatures), the role of nucleonic three-body forces, and the dependence of the direct URCA processes on the EoS.

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Critical temperature for the nuclear liquid-gas phase transition (from multifragmentation and fission)

Cited by 33 publications

References 36 publications

Functional renormalization group studies of nuclear and neutron matter

Functional renormalization group studies of nuclear and neutron matter

Dense nucleonic matter and the renormalization group

Nuclear Equation of State for Compact Stars and Supernovae

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