New equation of state for astrophysical simulations

Shen, Gang; Horowitz, C. J.; Teige, S.

doi:10.1103/physrevc.83.035802

Cited by 212 publications

(281 citation statements)

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“…The QS approach gives the Beth-Uhlenbeck formula in the low density limit, but gives also a generalized Beth-Uhlenbeck formula which takes in-medium effects into account [40]. The virial EOS of G. Shen et al [31,32] uses also the correct second virial coefficient so that the chemical constants are reduced, but mean-field effects are not included consistently so that the results for the chemical constants remain near to the values of the ideal NSE case. An attempt to construct an EOS which treats simultaneously the virial coefficient and the mean-field contributions has been performed in Ref.…”

Section: E Qsmentioning

confidence: 99%

“…At highest den-sity, a sudden decrease of K c [α] occurs, which is probably due to the onset of the transition from the "virial regime" to the intermediate density regime without alpha particles. Note that the tabulated EOSs of G. Shen et al are based on a smoothing and interpolation procedure [31,32], which could explain why the transition between the two regimes is smoothed out and not abrupt.…”

Section: G Shen Et Almentioning

confidence: 99%

“…The EOSs of G. Shen et al are available for two different RMF interactions, NL3 [31] and FSUgold [32]. Because the FSUgold parametrization lead to a maximum neutron star mass of only 1.7 M ⊙ , an additional phenomenological pressure contribution was introduced, leading to a sufficiently high maximum mass of 2.1 M ⊙ .…”

Section: G Shen Et Almentioning

confidence: 99%

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Constraining supernova equations of state with equilibrium constants from heavy-ion collisions

et al. 2015

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Cluster formation is a fundamental aspect of the equation of state (EOS) of warm and dense nuclear matter such as can be found in supernovae (SN). Similar matter can be studied in heavy-ion collisions (HIC). We use the experimental data of Qin et al. 2012 to test calculations of cluster formation and the role of in-medium modifications of cluster properties in SN EOSs. For the comparison between theory and experiment we use chemical equilibrium constants as the main observables. This reduces some of the systematic uncertainties and allows deviations from ideal gas behavior to be identified clearly. In the analysis, we carefully account for the differences between matter in SN and HIC. We find that, at the lowest densities, the experiment and all theoretical models are consistent with the ideal gas behavior. At higher densities ideal behavior is clearly ruled out and interaction effects have to be considered. The contributions of continuum correlations are of relevance in the virial expansion and remain a difficult problem to solve at higher densities. We conclude that at the densities and temperatures discussed mean-field interactions of nucleons, inclusion of all relevant light clusters, and a suppression mechanism of clusters at high densities have to be incorporated in the SN EOS.

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Section: E Qsmentioning

confidence: 99%

Section: G Shen Et Almentioning

confidence: 99%

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Constraining supernova equations of state with equilibrium constants from heavy-ion collisions

et al. 2015

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“…The SHT UU model consists of two NSs with gravitational mass of 1.4 M each, and employs the EOS by Shen, Horowitz, Teige (SHT, Shen et al 2010, Shen et al 2011. The initial NS spins are aligned with the orbital angular momentum, with dimensionless spin J/M 2 ≈ 0.125.…”

Section: Setup and Numerical Evolutionmentioning

confidence: 99%

The role of weak interactions in dynamic ejecta from binary neutron star mergers

Martin

Perego

Kastaun

et al. 2018

Class. Quantum Grav.

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Abstract. Weak reactions are critical for the neutron richness of the matter dynamically ejected after the merger of two neutron stars. The neutron richness, defined by the electron fraction (Y e ), determines which heavy elements are produced by the r-process and thus directly impacts the kilonova light curve. In this work, we have performed a systematic and detailed post-processing study of the impact of weak reactions on the distribution of the electron fraction and of the entropy on the dynamic ejecta obtained from an equal mass neutron star binary merger simulated in full general relativity and with microscopic equation of state. Previous investigations indicated that shocks increase Y e , however our results show that shocks can also decrease Y e , depending on their thermodynamical conditions. Moreover, we have found that neutrino absorption are key and need to be considered in future simulations. We also demonstrated that the angular dependence of the neutrino luminosity and the spatial distribution of the ejecta can lead to significant difference in the electron fraction distribution. In addition to the detailed study of the Y e evolution and its dependences, we have performed nucleosynthesis calculations. They clearly point to the necessity of improving the neutrino treatment in current simulations to be able to predict the contribution of neutron star mergers to the chemical history of the universe and to reliable calculate their kilonova light curves.

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“…The most frequently used EoS were developed by Lattimer and Swesty [6], based on the compressible liquid drop model and the non-relativistic Skyrme force , and by Shen et al, [7], who used the Thomas-Fermi (TF) approximation with a relativistic mean-field (RMF) model. Recently published new EoS for CCSN simulations [8,9] use the virial EoS at low density and Hartree RMF in both the inhomogeneous and uniform matter regions. Hempel et al [10] reported calculations based on the nuclear statistical equilibrium model, which includes excluded volume effects and RMF interactions.…”

mentioning

confidence: 99%