Nuclear Statistical Equilibrium equation of state for core collapse

Raduta, Ad. R.; Gulminelli, F.

doi:10.1016/j.nuclphysa.2018.11.003

Cited by 34 publications

(18 citation statements)

References 72 publications

(173 reference statements)

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“…Several NSE models and resulting EoS have been proposed in the last decade, see e.g. [38][39][40][41][42][43][44]. For the interaction between nucleons, different relativistic mean field models, Skyrme effective interactions or variational approaches have been employed that span significant ranges of nuclear matter parameters in both isovector and isoscalar channels, accounting thus well for present day uncertainties in the nuclear matter EoS.…”

Section: B Equations Of Statementioning

confidence: 99%

“…It has been shown that the latter point strongly influences the nuclear abundances under the thermodynamic conditions during collapse [13,14]. Additional differences exist in the identification of the bound and unbound part of nuclear clusters to define abundances, but this point did not sizably modify the EoS [41]. For further details, the reader is referred to [39,41].…”

Section: B Equations Of Statementioning

confidence: 99%

“…Additional differences exist in the identification of the bound and unbound part of nuclear clusters to define abundances, but this point did not sizably modify the EoS [41]. For further details, the reader is referred to [39,41].…”

Section: B Equations Of Statementioning

confidence: 99%

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Impact of electron capture rates for nuclei far from stability on core-collapse supernovae

et al. 2020

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The impact of electron-capture (EC) cross sections on neutron-rich nuclei on the dynamics of corecollapse during infall and early post-bounce is studied performing spherically symmetric simulations in general relativity using a multigroup scheme for neutrino transport and full nuclear distributions in extended nuclear statistical equilibrium models. We thereby vary the prescription for EC rates on individual nuclei, the nuclear interaction for the EoS, the mass model for the nuclear statistical equilibrium distribution and the progenitor model. In agreement with previous works, we show that the individual EC rates are the most important source of uncertainty in the simulations, while the other inputs only marginally influence the results. A recently proposed analytic formula to extrapolate microscopic results on stable nuclei for EC rates to the high densities and temperatures and the neutron rich region, with a functional form motivated by nuclear-structure data and parameters fitted from large scale shell model calculations, is shown to lead to a sizable (16%) reduction of the electron fraction at bounce compared to more primitive prescriptions for the rates, leading to smaller inner core masses and slower shock propagation. We show that the EC process involves ≈ 130 different nuclear species around 86 Kr mainly in the N = 50 shell closure region, and establish a list of the most important nuclei to be studied in order to constrain the global rates.

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Section: B Equations Of Statementioning

confidence: 99%

Section: B Equations Of Statementioning

confidence: 99%

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Impact of electron capture rates for nuclei far from stability on core-collapse supernovae

et al. 2020

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“…For this work, we will use two different EoS models. As a fiducial case for which we will calculate neutrino opacities in RPA, we will consider the NSE model of Raduta and Gulminelli [48,49] named "RG(SLy4)". It employs the non-relativistic SLy4 [50] Skyrme interaction for nucleons.…”

Section: Equation Of Statementioning

confidence: 99%

Improved neutrino-nucleon interactions in dense and hot matter for numerical simulations

et al. 2020

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Neutrinos play an important role in compact star astrophysics: neutrino-heating is one of the main ingredients in core-collapse supernovae, neutrino-matter interactions determine the composition of matter in binary neutron star mergers and have among others a strong impact on conditions for heavy element nucleosynthesis and neutron star cooling is dominated by neutrino emission except for very old stars. Many works in the last decades have shown that in dense matter medium effects considerably change the neutrino-matter interaction rates, whereas many astrophysical simulations use analytic approximations which are often far from reproducing more complete calculations. In this work we present a scheme which allows to incorporate improved rates for charged current interactions, into simulations and show as an example some results for core-collapse supernovae, where a noticeable difference is found in the location of the neutrinospheres of the low-energy neutrinos in the early post-bounce phase.

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“…In particular, in the outer layers of the exploding star, the thermodynamic conditions are such that strong (but not weak) equilibrium is established and matter is clusterized. To describe subsaturation supernova and early proto-neutron star matter, in the recent years, a number of improved equation of state (EoS) models has been proposed that include the full nuclear distribution [2][3][4][5][6][7][8][9][10][11][12][13][14], but only a few of them have been used to produce tables which are publicly available [15]. Exploring the effect of the different microscopic ingredients and their uncertainties is not always simple in these models, because the impact of the energy functional can be hardly decoupled from the many-body description of the clusters, which is not the same in the different models.…”

Section: Introductionmentioning

confidence: 99%

Isospin properties of the pasta phase with an extended statistical model from microscopic energy functionals

2020

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In this work, we have developed an extended statistical model to study nuclear multifragmentation reactions at intermediate energies, and we link the associated observables to the properties of supernova matter. The canonical thermodynamical model, used for this study, is modified by including inputs from the relativistic mean-field energy functionals. Even though the length scale of the supernova matter is very large compared to that of the multifragmentation reaction, we find an isospin observable, the average Z/N of the fragments, which is almost independent of the size of system, and can be directly compared to the estimation of fractionation in infinite nuclear matter. The isospin ratio Z/N of the heaviest cluster produced in nuclear fragmentation and of the corresponding pasta structure occurring in supernova matter are significantly lower than the spinodal estimation in uncharged nuclear matter, due to the presence of lighter isospin symmetric clusters that dominate the mass fraction in full equilibrium at finite temperature. The screening effect of electrons is also studied.

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Nuclear Statistical Equilibrium equation of state for core collapse

Cited by 34 publications

References 72 publications

Impact of electron capture rates for nuclei far from stability on core-collapse supernovae

Impact of electron capture rates for nuclei far from stability on core-collapse supernovae

Improved neutrino-nucleon interactions in dense and hot matter for numerical simulations

Isospin properties of the pasta phase with an extended statistical model from microscopic energy functionals

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