Light clusters, pasta phases, and phase transitions in core-collapse supernova matter

Pais, Helena; Chiacchiera, Silvia; Providência, Constança

doi:10.1103/physrevc.91.055801

Cited by 56 publications

(77 citation statements)

References 48 publications

(119 reference statements)

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“…We note that the deuteron clustering discussed above does not describe the realistic deuteron mixing in hot dilute nuclear matter as treated in recent other supernova EOS tables [23,30,31,32] for the following reasons: i) Since we employ the frozen correlation approximation in our variational calculation, the deuteron-type strong correlations at zero temperature survive even at finite temperatures, while most deuterons would be destroyed in realistic hot supernova matter. ii) In the case of light nuclei such as deuterons, the energy contribution from the center-of-mass motion would be important.…”

Section: Modification Of the Eos Of Uniform Nuclear Matter At Low Denmentioning

confidence: 99%

“…In our project to construct a new supernova EOS, we employ the prescription for the calculation of non-uniform nuclear EOS used by Shen et al, i.e., we calculate nuclides in a Wigner-Seitz cell in the Thomas-Fermi approximation. Though several other Thomas-Fermi calculations for hot nuclear matter have also been adopted especially for the study of the pasta phase [21,22,23], we employ the Thomas-Fermi calculation originally adopted by Shen et al as one of the standard Thomas-Fermi calculations for supernova EOS.…”

Section: Introductionmentioning

confidence: 99%

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Nuclear equation of state for core-collapse supernova simulations with realistic nuclear forces

et al. 2017

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A new table of the nuclear equation of state (EOS) based on realistic nuclear potentials is constructed for core-collapse supernova numerical simulations. Adopting the EOS of uniform nuclear matter constructed by two of the present authors with the cluster variational method starting from the Argonne v18 and Urbana IX nuclear potentials, the Thomas-Fermi calculation is performed to obtain the minimized free energy of a Wigner-Seitz cell in non-uniform nuclear matter. As a preparation for the Thomas-Fermi calculation, the EOS of uniform nuclear matter is modified so as to remove the effects of deuteron cluster formation in uniform matter at low densities. Mixing of alpha particles is also taken into account following the procedure used by Shen et al. ( , 2011. The critical densities with respect to the phase transition from non-uniform to uniform phase with the present EOS are slightly higher than those with the Shen EOS at small proton fractions. The critical temperature with respect to the liquid-gas phase transition decreases with the proton fraction in a more gradual manner than in the Shen * Corresponding author Email address: hajime.togashi@riken.jp (H. Togashi)Preprint submitted to Nuclear Physics A March 23, 2017EOS. Furthermore, the mass and proton numbers of nuclides appearing in non-uniform nuclear matter with small proton fractions are larger than those of the Shen EOS. These results are consequences of the fact that the density derivative coefficient of the symmetry energy of our EOS is smaller than that of the Shen EOS.

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Section: Modification Of the Eos Of Uniform Nuclear Matter At Low Denmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Nuclear equation of state for core-collapse supernova simulations with realistic nuclear forces

et al. 2017

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“…The pasta phase calculation (see, e.g., [20] and references therein) is done by considering two different methods: the coexisting-phases (CP) approximation, where the Gibbs equilibrium conditions are used to get the lowest free-energy state and the surface and Coulomb terms are added "by hand," and the compressible liquid drop (CLD) model, where, unlike the CP approximation, both the Coulomb and surface terms are taken into account in the minimization of the total energy of the system.…”

Section: Introductionmentioning

confidence: 99%

Neutron stars: From the inner crust to the core with the (extended) Nambu–Jona-Lasinio model

2016

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Nucleonic matter is described within an SU(2) extended Nambu-Jona-Lasinio (NJL) model. Several parametrizations with different nuclear matter saturation properties are proposed. At subsaturation, nuclear pasta phases are calculated within two methods: the coexistence-phases approximation and the compressible liquid drop model, with the surface tension coefficient determined using a geometrical approach at zero temperature. A unified equation of state of stellar matter for the inner crust, with the nuclear pasta phases, and the core is calculated. The mass and radius of neutron stars within this framework are obtained for several families of hadronic and hybrid stars. The quark phase of hybrid stars is described within the SU(3) NJL model including a vector term. Stellar macroscopic properties are in accordance with some of the recent results in the literature.

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“…The topics of current interest are, for example, the improvements on the supernova and warm neutron star equations of state and thermodynamics [7,8] which include the multi-cluster composition of matter [9,10,11,12,13,14,15,16,17,18,19,20,21]. Another aspect of the problem is the effects of light clusters in intermediate energy heavy ion collisions [22,23,24,25,26,27] which were extensively studied using various methods, see for example [28,29,30].…”

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confidence: 99%

Composition of Nuclear Matter with Light Clusters and Bose–Einstein Condensation of $$\alpha $$ α Particles

et al. 2017

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The Bose-Einstein condensation of α partciles in the multicomponent environment of dilute, warm nuclear matter is studied. We consider the cases of matter composed of light clusters with mass numbers A ≤ 4 and matter that in addition these clusters contains 56 Fe nuclei. We apply the quasiparticle gas model which treats clusters as bound states with infinite life-time and binding energies independent of temperature and density. We show that the α particles can form a condensate at low temperature T ≤ 2 MeV in such matter in the first case. When the 56 Fe nucleus is added to the composition the cluster abundances are strongly modified at low temperatures, with an important implication that the α condensation at these temperatures is suppressed.

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Light clusters, pasta phases, and phase transitions in core-collapse supernova matter

Cited by 56 publications

References 48 publications

Nuclear equation of state for core-collapse supernova simulations with realistic nuclear forces

Nuclear equation of state for core-collapse supernova simulations with realistic nuclear forces

Neutron stars: From the inner crust to the core with the (extended) Nambu–Jona-Lasinio model

Composition of Nuclear Matter with Light Clusters and Bose–Einstein Condensation of $$\alpha $$ α Particles

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