2013
DOI: 10.48550/arxiv.1303.0064
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The NDL Equation of State for Supernova Simulations

Abstract: We present an updated and improved equation of state (which we call the NDL EoS) for use in neutron-star structure and supernova simulations. This EoS is based upon a framework originally developed by Bowers & Wilson, but there are numerous changes. Among them are: (1) a reformulation in the context of density functional theory; (2) the possibility of the formation of material with a net proton excess (Ye > 0.5); (3) an improved treatment of the nuclear statistical equilibrium and the transition to heavy nucle… Show more

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Cited by 5 publications
(7 citation statements)
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“…In Fig. 4, we show the comparison of the J 0 constraint obtained in our analysis with those obtained with other analyses and/or other methods ( [22,25,63,64]), including the constraint of J 0 = −700 ± 500 MeV obtained by [63] from the analysis of nuclear GMR, the constraint of J 0 = −280 +72 −410 (−500 +170 −290 ) MeV obtained by [64] from analyzing a heterogeneous data set of six neutron stars using a Markov chain Monte Carlo algorithm within a Bayesian framework by assuming r ph ≫ R (r ph = R) where r ph is the photospheric radius at the time the flux is evaluated and R is the stellar radius, the constraint of J 0 = −355 ± 95 MeV deduced by [25] based on a correlation analysis method within SHF energy density functional, and the constraint of J 0 = −390±90 MeV deduced [22] who used the similar method as [25]. It is seen that the constrained region of J 0 obtained in the present work has a remarkable overlap with those existing in the literature.…”
Section: Resultsmentioning
confidence: 90%
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“…In Fig. 4, we show the comparison of the J 0 constraint obtained in our analysis with those obtained with other analyses and/or other methods ( [22,25,63,64]), including the constraint of J 0 = −700 ± 500 MeV obtained by [63] from the analysis of nuclear GMR, the constraint of J 0 = −280 +72 −410 (−500 +170 −290 ) MeV obtained by [64] from analyzing a heterogeneous data set of six neutron stars using a Markov chain Monte Carlo algorithm within a Bayesian framework by assuming r ph ≫ R (r ph = R) where r ph is the photospheric radius at the time the flux is evaluated and R is the stellar radius, the constraint of J 0 = −355 ± 95 MeV deduced by [25] based on a correlation analysis method within SHF energy density functional, and the constraint of J 0 = −390±90 MeV deduced [22] who used the similar method as [25]. It is seen that the constrained region of J 0 obtained in the present work has a remarkable overlap with those existing in the literature.…”
Section: Resultsmentioning
confidence: 90%
“…The exact knowledge on the EOS of ANM provides important information on the in-medium nuclear effective interactions which play a central role in understanding the structure and decay properties of finite nuclei as well as the related dynamical problems in nuclear reactions ( [1][2][3][4][5][6][7][8][9][10][11][12][13][14][15][16]). The EOS of ANM also plays a decisive role in understanding a number of important issues in astrophysics including the structure and evolution of neutron stars as well as the mechanism of supernova explosion ( [17][18][19][20][21][22][23]). Conventionally, the EOS of ANM is given by the binding energy per nucleon as functions of nucleon density ρ and isospin asymmetry δ, i.e., E(ρ, δ), and some bulk characteristic parameters defined at the saturation density ρ 0 of symmetric nuclear matter (SNM) are usually introduced to quantitatively characterize the EOS of ANM.…”
Section: Introductionmentioning
confidence: 99%
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“…The incompressibility K 0 of SNM has been extensively investigated [33,41], and the most widely used values are K 0 = 240 ± 20 MeV [36,37] or 230 ± 40 MeV [38]. However, the skewness coefficient J 0 is still poorly known [42][43][44][45][46][47]. In Fig.…”
Section: The Lower Boundary Of Nuclear Symmetry Energy Constrained By...mentioning
confidence: 99%
“…MeV in the HMT model. Unfortunately, our current knowledge on the parameter Q 0 [74][75][76][77][78][79][80] is still too poor to put a constraint on it. On the other hand, the pressure of SNM in the density range of about 2ρ 0 to 5ρ 0 has been experimentally constrained by measuring nuclear collective flows in heavy-ion collisions [3], which is shown as a cyan band in the right panel of Fig.…”
Section: Validation Of Src-modified Single-nucleon Momentum Distribut...mentioning
confidence: 99%