A comparative study of statistical models for nuclear equation of state of stellar matter

Buyukcizmeci, N.; Botvina, A. S.; Mishustin, I. N.; Ogul, R.; Hempel, M.; Schaffner-Bielich, J.; Thielemann, F. -K.; Furusawa, S.; Sumiyoshi, K.; Yamada, S.; Suzuki, H.

doi:10.48550/arxiv.1211.5990

Cited by 4 publications

(8 citation statements)

References 63 publications

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“…5, for all temperatures below the critical one the low k behavior is governed by the Fisher exponent τ and by the surface term which is proportional to ξ 2 , whereas at large values of k the fragment size attenuation is solely determined by the bulk term which is proportional to ξ 1 . These fragment size distributions are qualitatively similar to that ones found recently in [46] for the nuclear matter EoS neutralized by the electrons in the stellar environments. A true power law of the fragment size distribution corresponds to the tricritical endpoint, for ξ 1 = 0 and ξ 2 = 0.…”

Section: Manifestation Of Negative Surface Tension Valuessupporting

confidence: 88%

“…At the tricritical point about 65 % of the matter belongs to the liquid fragment, while the rest belongs to the gas, which demonstrates a clear power law. Such a behavior of the fragment size distributions in the mixed phase is qualitatively similar to the one found in [46] inside the mixed phase, see Figs. 4 and 6 in [46].…”

Section: Manifestation Of Negative Surface Tension Valuessupporting

confidence: 78%

“…Such a behavior of the fragment size distributions in the mixed phase is qualitatively similar to the one found in [46] inside the mixed phase, see Figs. 4 and 6 in [46]. The main difference with the results of [46] is that the present model employes the grand canonical ensemble in thermodynamic limit, whereas [46] is dealing with the canonical ensemble for a finite system.…”

Section: Manifestation Of Negative Surface Tension Valuessupporting

confidence: 78%

“…In order to make a comparison with the results reported in [46] we have normalized the fragment size distributions in the mixed phase to the total number of 500 nucleons. In Fig.…”

Section: Manifestation Of Negative Surface Tension Valuesmentioning

confidence: 99%

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The statistical multifragmentation model for liquid–gas phase transition with a compressible nuclear liquid

Sagun¹,

Ivanytskyi²,

Bugaev

et al. 2014

Nuclear Physics A

148

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We propose a new formulation of the statistical multifragmentation model based on the analysis of the virial expansion for a system of the nuclear fragments of all sizes. The developed model not only enables us to account for short-range repulsion, but also to calculate the surface free energy which is induced by the interaction between the fragments. We propose a new parameterization for the liquid phase pressure which allows us to introduce a compressible nuclear liquid into the statistical multifragmentation model. The resulting model is exactly solvable and has no irregular behavior of the isotherms in the mixed phase region that is typical for mean-field models. The general conditions for the 1-st and 2-nd (or higher) order phase transitions are formulated. It is shown that all endpoints of the present model phase diagram are the tricritical points, if the Fisher exponent τ is in the range 3 2 ≤ τ ≤ 2. The treatment of nuclear liquid compressibility allows us to reduce the tricritical endpoint density of the statistical multifragmentation model to one third of the normal nuclear density. A specific attention is paid to of the fragment size distributions in the region of a negative surface tension at supercritical temperatures.

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Section: Manifestation Of Negative Surface Tension Valuessupporting

confidence: 88%

Section: Manifestation Of Negative Surface Tension Valuessupporting

confidence: 78%

Section: Manifestation Of Negative Surface Tension Valuessupporting

confidence: 78%

“…In order to make a comparison with the results reported in [46] we have normalized the fragment size distributions in the mixed phase to the total number of 500 nucleons. In Fig.…”

Section: Manifestation Of Negative Surface Tension Valuesmentioning

confidence: 99%

See 2 more Smart Citations

The statistical multifragmentation model for liquid–gas phase transition with a compressible nuclear liquid

Sagun¹,

Ivanytskyi²,

Bugaev

et al. 2014

Nuclear Physics A

148

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“…On the other hand, below ρ 0 , we use the thermal EOS which consists of an ensemble of nuclei and interacting nucleons in nuclear statistical equilibrium given by Hempel and Schaffner-Bielich (HS EOS) [62]. (Use of other EOSs below ρ 0 does not show quantitative difference as discussed in [63]. ) Once the baryon density becomes smaller than the neutron drip density 10 −3 ρ 0 , the temperature becomes smaller than 0.1 MeV.…”

Section: Neutron Star With Crover Eos At T =mentioning

confidence: 99%

Hyperon puzzle, hadron-quark crossover and massive neutron stars

2016

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Abstract. Bulk properties of cold and hot neutron stars are studied on the basis of the hadron-quark crossover picture where a smooth transition from the hadronic phase to the quark phase takes place at finite baryon density. By using a phenomenological equation of state (EOS) "CRover" which interpolates the two phases at around 3 times the nuclear matter density (ρ0), it is found that the cold NSs with the gravitational mass larger than 2M can be sustained. This is in sharp contrast to the case of the first-order hadron-quark transition. The radii of the cold NSs with the CRover EOS are in the narrow range (12.5±0.5) km which is insensitive to the NS masses. Due to the stiffening of the EOS induced by the hadron-quark crossover, the central density of the NSs is at most 4 ρ0 and the hyperon-mixing barely occurs inside the NS core. This constitutes a solution of the long-standing hyperon puzzle. The effect of color superconductivity (CSC) on the NS structures is also examined with the hadron-quark crossover. For the typical strength of the diquark attraction, a slight softening of the EOS due to two-flavor CSC (2SC) takes place and the maximum mass is reduced by about 0.2 M . The CRover EOS is generalized to the supernova matter at finite temperature to describe the hot NSs at birth. The hadron-quark crossover is found to decrease the central temperature of the hot NSs under isentropic condition. The gravitational energy release and the spin-up rate during the contraction from the hot NS to the cold NS are also estimated.PACS. 21.65.Qr Quark matter -26.60.-c Nuclear matter aspects of neutron stars -97.60.Jd Neutron Stars

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Hadron–quark crossover and hot neutron stars at birth

Masuda

Hatsuda

Takatsuka

2016

Prog. Theor. Exp. Phys.

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We construct a new isentropic equation of state (EOS) at finite temperature "CRover" on the basis of the hadron-quark crossover at high density. By using the new EOS, we study the structure of hot neutron stars at birth with the typical lepton fraction (Y l = 0.3 − 0.4) and the typical entropy per baryon (Ŝ = 1 − 2). Due to the gradual appearance of quark degrees of freedom at high density, the temperature T and the baryon density ρ at the center of the hot neutron stars with the hadron-quark crossover are found to be smaller than those without the crossover by a factor of 2 or more. Typical energy release due to the contraction of a hot neutron star to a cold neutron star with the mass M = 1.4M ⊙ is shown to be about 0.04M ⊙ with the spin-up rate about 14 %.Introduction: In the core-collapsed Type-II supernova explosion, the proto-neutron star (PNS) with the radius ∼ 100−200 km is formed. During the first few seconds after the core bounce, the PNS undergoes a rapid contraction and evolves into either a "hot" neutron star (NS) with the radius ∼ 10−20 km or a black hole. The hot NS at birth in quasihydrostatic equilibrium is composed of the supernova matter with the typical lepton fraction, Y l = Y e + Y ν ∼ 0.3 − 0.4, and the typical entropy per baryon 1 ,Ŝ ∼ 1 − 2: They are caused by the neutrino trapping at the baryon density ρ exceeding 10 12 g/cm 3 . With this as an initial condition, the hot NS contracts gradually by the neutrino diffusion with the time scale of several tens of seconds and evolves to a nearly "cold" NS with Y ν ≃ 0 andŜ ≃ 0), unless another collapse to a black hole does not take place [1][2][3].The hot neutron star provides us with various information on the properties and dynamics of high density matter [4,5]. The purpose of this Letter is to study the hot neutron star at birth with degenerate neutrinos on the basis of an equation of state (EOS) "CRover" at finite temperature T which is newly developed on the basis of the hadron-quark crossover picture at high baryon densities. Such an EOS for "cold" neutron-star matter has been previously studied by the present authors [6,7]: It was shown that a smooth crossover from the hadronic matter to the strongly-interacting quark matter around ρ ∼ 3ρ 0 (ρ 0 = 0.17/fm 3 being the normal nuclear matter density) can support the cold neutron star with the maximum mass

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A comparative study of statistical models for nuclear equation of state of stellar matter

Abstract: We compare three different statistical models for the equation of state (EOS) of stellar matter at subnuclear densities and temperatures (0.5-10 MeV) expected to

Cited by 4 publications

References 63 publications

The statistical multifragmentation model for liquid–gas phase transition with a compressible nuclear liquid

The statistical multifragmentation model for liquid–gas phase transition with a compressible nuclear liquid

Hyperon puzzle, hadron-quark crossover and massive neutron stars

Hadron–quark crossover and hot neutron stars at birth

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