Relativistic Equation of State for Core-Collapse Supernova Simulations

# Relativistic Equation of State for Core-Collapse Supernova Simulations

## Abstract

We construct the equation of state (EOS) of dense matter covering a wide range of temperature, proton fraction, and density for the use of core-collapse supernova simulations. The study is based on the relativistic mean-field (RMF) theory, which can provide an excellent description of nuclear matter and finite nuclei. The Thomas–Fermi approximation in combination with assumed nucleon distribution functions and a free energy minimization is adopted to describe the non-uniform matter, which is composed of a lattice of heavy nuclei. We treat the uniform matter and non-uniform matter consistently using the same RMF theory. We present two sets of EOS tables, namely EOS2 and EOS3. EOS2 is an update of our earlier work published in 1998 (EOS1), where only the nucleon degree of freedom is taken into account. EOS3 includes additional contributions from hyperons. The effect of hyperons on the EOS is negligible in the low-temperature and low-density region, whereas it tends to soften the EOS at high density. In comparison with EOS1, EOS2 and EOS3 have an improved design of ranges and grids, which covers the temperature range MeV with the logarithmic grid spacing (92 points including ), the proton fraction range with the linear grid spacing (66 points), and the density range with the logarithmic grid spacing (110 points).

equation of state — stars: neutron — supernovae: general
Online-only material: color figures, machine-readable tables

## 1 Introduction

The equation of state (EOS) of dense matter plays an important role in various astrophysical phenomena such as supernova explosions and the formation of neutron stars and black holes (Janka et al., 2007; Burrows et al., 2006; Sumiyoshi et al., 2005, 2009). Simulations of core-collapse supernovae cover a wide range of thermodynamic conditions, and extremely high density and temperature may be achieved when black holes are formed by failed supernovae. The temperature may vary from to more than MeV, the proton fraction changes from to around , and the density can vary from to more than . Clearly, it is very difficult to construct a complete EOS over such a wide range of parameters. The information of matter under extreme conditions is far beyond our knowledge of nuclear physics from laboratory experiments. Therefore, it is necessary to perform a large extrapolation based on a theoretical model that is supported by microscopic theory and consistent with available experimental data. During the past few decades, great efforts have been made to study the EOS of nuclear matter (Lattimer & Swesty, 1991; Schaffner & Mishustin, 1996; Weber, 2005; Lattimer & Prakash, 2007). However, most of the investigations focused on detailed aspects of nuclear matter, which were often restricted to the case of zero temperature or high density with uniform distribution of particles. This kind of EOS is generally not applicable for use in supernova simulations. So far, there exist only two realistic EOSs which are commonly used in simulations of core-collapse supernovae, namely the one by Lattimer & Swesty (1991) and the one by Shen et al. (1998b). The Lattimer–Swesty EOS is based on a compressible liquid-drop model with a Skyrme force. The Shen EOS is based on a relativistic mean-field (RMF) model and uses the Thomas–Fermi approximation with assumed nucleon distribution functions in a Wigner–Seitz cell for the description of non-uniform matter. Recently, a Hartree mean-field calculation (Shen et al., 2010a) was performed for the Wigner–Seitz cell instead of the Thomas–Fermi approximation used by Shen et al. (1998b). The Hartree calculation can incorporate nuclear shell effects, but it requires much more computational resources.

In our earlier work (Shen et al., 1998a, b), we constructed the relativistic EOS for supernova simulations, which has been widely used in astrophysical simulations over the past decade (Janka et al., 2007; Burrows et al., 2006; Sumiyoshi et al., 2005; Sagert et al., 2009). The EOS is based on the RMF theory combined with the Thomas–Fermi approximation. The RMF theory with nonlinear and terms is able to reproduce nuclear matter saturation properties and provide a good description for both stable and unstable nuclei (Sugahara & Toki, 1994a; Hirata et al., 1996). The Thomas–Fermi approximation in combination with assumed nucleon distribution functions and a free energy minimization is adopted to describe the non-uniform matter which is modeled as a mixture of a single species of heavy nuclei, alpha particles, and free nucleons that exist outside of nuclei, while the leptons can be treated as uniform non-interacting particles separately. The RMF results are taken as input in the Thomas–Fermi calculation, so the treatments of non-uniform matter and uniform matter in this EOS are sufficient to obtain the table in a consistent manner. It would be preferable to treat the mixture of nuclei as recently done in Hempel & Schaffner-Bielich (2010)Furusawa et al. (2011), and Blinnikov et al. (2011) for the detailed treatment of electron captures on nuclei in supernova core. However, it is beyond the scope of the current update of the Shen EOS table, which has been routinely used in astrophysical simulations.

Toward a more efficient and effective use of the Shen EOS table, we are required to make improvements in the EOS given in Shen et al. (1998b), hereafter referred to as EOS1. The main demand is to increase the number of temperature points which is crucial in the simulation of core-collapse supernovae. In some cases, the temperature may reach more than MeV, so it is encouraged to provide results at some higher temperatures although it is probably beyond the applicability of the RMF theory. It is generally believed that at sufficiently high temperature and/or density nuclear matter undergoes a phase transition to quark–gluon plasma (QGP). Based on experimental data from high-energy heavy ion collisions and lattice quantum chromodynamics (QCD) calculations, it is known that the critical temperature for the QCD phase transition is around MeV for zero baryon density (Gupta et al., 2011). Therefore, we note that the nuclear EOS at extremely high temperature and/or density is not reliable due to the QCD phase transition, although results of the RMF theory are provided for practical use in astrophysical simulations. Another suggestion is to use a linear grid for the proton fraction , instead of the logarithmic grid used in EOS1, which can add more points in the important region for supernova simulations and save memory space by reducing the number of points at . Furthermore, a proton-rich matter may be involved in astrophysical simulations (Pruet et al., 2005; Fröhlich et al., 2006), and therefore the information at is needed. In EOS1, the density grid spacing is only approximately equal at high density, it is now possible to perform the calculation with equal grid spacing in the whole range of density. Since it is desirable and feasible to make these improvements, we work out a new version of the EOS table, hereafter referred to as EOS2, which contains the same degrees of freedom as EOS1.

In recent years, there has been extensive discussion in the literature on the influence of non-nucleonic degrees of freedom in dense matter (Weber, 2005; Lattimer & Prakash, 2007). It is generally believed that hyperons appear around twice normal nuclear matter density in cold neutron star matter (Schaffner & Mishustin, 1996; Shen, 2002; Ishizuka et al., 2008). The first hyperon to appear is that is the lightest one with an attractive potential in nuclear matter (Ishizuka et al., 2008; Yue et al., 2009). hyperons are now considered to appear at a higher density than , because hyperons feel a repulsive potential in nuclear matter according to recent developments in hypernuclear physics (Ishizuka et al., 2008). In the work of Ishizuka et al. (2008), the authors examined the properties of dense matter based on an extended RMF model including the full baryon octet. They presented several sets of EOS including hyperons for simulations of core-collapse supernovae, which were connected with EOS1 at low density in the simple procedure described in Section 2.3 of their paper. The effect of -wave pion condensation was also examined in Ishizuka et al. (2008), where the authors considered free thermal pions assuming the pion mass could not be affected by the interaction. In Ohnishi et al. (2009), the authors examined the possibility of -wave pion condensation in dense matter by using the phenomenological optical potentials determined from the pionic atom or pion–nucleus scattering data, and they concluded that -wave pion condensation would hardly take place in neutron stars and especially have no chance if hyperons could participate in neutron star matter. The presence of boson condensation and deconfined quarks in neutron stars has been extensively discussed in many works (Schaffner & Mishustin, 1996; Weber, 2005; Lattimer & Prakash, 2007; Yang & Shen, 2008). It has been suggested that the quark matter may exist in the core of massive neutron stars, and the hadron–quark phase transition can proceed through a mixed phase of hadronic and quark matter (Glendenning, 1992; Weber, 2005; Lattimer & Prakash, 2007; Yang & Shen, 2008). If deconfined quark matter does exist inside stars, it is likely to be in a color superconducting phase, and various color superconducting phases have been intensively investigated in recent years (Buballa, 2005; Paulucci et al., 2011). In the works of Nakazato et al. (2008, 2010) and Sagert et al. (2009, 2010), the authors constructed the EOS tables for simulations of core-collapse supernovae including the hadron–quark phase transition at high density, which were connected with EOS1 at low density. The hadron–quark phase transition proceeded through a mixed phase obtained by the Gibbs conditions for phase equilibrium, where the RMF model was used for the hadronic phase and the bag model was adopted for the quark phase. Generally, the introduction of non-nucleonic degrees of freedom leads to a softening of the EOS and thereby a corresponding reduction in the maximum mass of neutron stars. The recent measurement of the Shapiro delay in the radio pulsar PSR J1614-2230 yielded a mass of  (Demorest et al., 2010). Such a high neutron star mass provides an important constraint on the EOS at high density and rules out many predictions of non-nucleonic components in neutron star interiors. However, it is currently difficult to rule out all possible exotica with the observation, some theoretical calculations including hyperons and/or quarks could be compatible with the observation of PSR J1614-2230 (Lattimer & Prakash, 2007, 2010; Stone et al., 2007; Paulucci et al., 2011).

Among these exotic candidates, hyperons are the most likely to occur in dense matter. In addition, much more experimental information is now available for than other hyperons (Takahashi et al., 2001; Nakazawa et al., 2010). From the experimental binding energies of single- hypernuclei, the potential depth of in nuclear matter is estimated to be around MeV (Shen et al., 2006). Several recent observations of double- hypernuclei (see Table 4 of Nakazawa et al. (2010)) indicate that the effective interaction should be considerably weaker than that deduced from the earlier measurement (Hiyama, 2010). In theoretical studies of hypernuclei, the RMF theory with nonlinear and terms is able to provide a reasonable description of single- and double- hypernuclei (Shen et al., 2006). The influence of hyperons on neutron star properties has been investigated within the RMF model (Sugahara & Toki, 1994b). We would like to examine the effect of hyperons on the EOS for simulations of core-collapse supernovae, while other hyperons such as and are ignored due to their relatively high threshold densities and lack of available experimental data. We construct the relativistic EOS with the inclusion of hyperons, hereafter referred to as EOS3. For the contribution of hyperons in EOS3, we assume that the equilibrium condition is valid. In a supernova explosion, the dynamical timescale is of the order of milliseconds, which is long enough to establish equilibrium with respect to weak interactions that change strangeness on the timescale of microseconds or less (Sagert et al., 2009, 2010). In fact, hyperons can have a noticeable effect on the properties of matter mainly at high density. It is known that weak equilibrium could be achieved at densities above where neutrinos begin to be trapped in the core (Kotake et al., 2006; Janka et al., 2007). Therefore, it is justified to use the equilibrium condition to determine the fraction of supernova matter at high density where hyperons have a noticeable contribution. In the work of Ishizuka et al. (2008), the authors assumed weak equilibrium among the full baryon octet when they determined the composition of supernova matter at a fixed density, temperature, and charge fraction. They examined the appearance of hyperons during the evolution of core collapse and bounce, and found that the effect of hyperons would be small in a spherical and adiabatic collapse of a star by the hydrodynamics without neutrino transfer (Ishizuka et al., 2008). The hyperons are expected to appear and play an important role in the thermal evolution of protoneutron stars and the black hole formation from massive stars (Pons et al., 1999; Sumiyoshi et al., 2009).

We have two aims in this paper. The first is to improve the EOS table according to the requirements of the users. In comparison with the earlier version (EOS1), the following improvements are made in EOS2 and EOS3 (see Table 1 for details of the comparison).

• The number of points is largely increased, the upper limit of is extended, and equal grid spacing for is used.

• A linear grid is adopted instead of the logarithmic grid used in EOS1 and the upper limit is extended.

• The upper limit of is extended and equal grid spacing is used in the whole range of , whereas it is only approximately equal at high density in EOS1.

The finer grids are favorable for better accuracy in the numerical simulations of core-collapse supernovae. The wide coverage of the conditions is necessary for numerical simulations of astrophysical phenomena including black hole formation, neutron star mergers, and nucleosynthesis. The second aim of this paper is to provide the EOS table with the inclusion of hyperons for the use in simulations of core-collapse supernovae. The difference between EOS2 and EOS3 is that the contribution from hyperons is included in EOS3 when the fraction is larger than .

This paper is arranged as follows. In Section 2, we briefly describe the framework to calculate the EOS table. We introduce the RMF model with the inclusion of hyperons and explain how to determine the RMF parameters. To make this paper self-contained, we give a brief description of the Thomas–Fermi approximation for the non-uniform matter. In Section 3, we discuss our results without and with the inclusion of hyperons. We explore the properties of dense matter by examining the phase diagram, compositions, and thermodynamic quantities. Section 4 is devoted to a summary. In Appendix A, we give the definitions of the physical quantities tabulated in the EOS. EOS2 and EOS3 are presented in electronic tables and can also be found on several Web sites. In Appendix B, we describe various checks made for the EOS tables.

## 2 Model descriptions

We construct the EOS within the RMF framework (Serot & Walecka, 1986; Shen et al., 1998a, b, 2006). For uniform matter without heavy nuclei formed, the RMF theory can be easily used to calculate the properties of matter. For non-uniform matter where heavy nuclei are formed in order to lower the free energy, we adopt the Thomas–Fermi approximation based on the work by Oyamatsu (1993). The non-uniform matter can be modeled as a mixture of a single species of heavy nuclei, alpha particles, and free nucleons that exist outside of nuclei. The results of the RMF model are taken as input in the Thomas–Fermi calculation, so the treatments of non-uniform matter and uniform matter in this EOS are sufficient to obtain the table in a consistent manner. It would be preferable to treat the mixture of nuclei as recently done in Hempel & Schaffner-Bielich (2010)Furusawa et al. (2011), and Blinnikov et al. (2011) for the detailed treatment of electron captures on nuclei in supernova core. However, it is beyond the scope of the current update of the Shen EOS table, which has been routinely used in astrophysical simulations.

### 2.1 Relativistic mean-field theory

We adopt the RMF theory with nonlinear and terms to describe homogeneous nuclear matter (Sugahara & Toki, 1994a; Shen et al., 2006). We study the two cases without and with hyperons. In the RMF approach, baryons interact through the exchange of various effective mesons. The exchanged mesons considered in this work include isoscalar scalar and vector mesons ( and ) and an isovector vector meson (). In some published studies (Schaffner & Mishustin, 1996; Shen et al., 2006; Yue et al., 2009), the two hidden-strangeness () scalar and vector mesons ( and ) were included in a hyperon-rich system. It has been found that the attraction from exchange is almost canceled by the repulsion from exchange (Shen et al., 2006). Therefore, we neglect the contribution from the exchange of these two hidden-strangeness mesons in this work.

 LRMF = ¯ψ[iγμ∂μ−M−gσσ−gωγμωμ−gργμτaρaμ]ψ (1) +¯ψΛ[iγμ∂μ−MΛ−gΛσσ−gΛωγμωμ]ψΛ +12∂μσ∂μσ−12m2σσ2−13g2σ3−14g3σ4 −14WμνWμν+12m2ωωμωμ+14c3(ωμωμ)2 −14RaμνRaμν+12m2ρρaμρaμ,

where and denote the nucleon and hyperon fields, respectively. , , and are , , and meson fields with masses , , and . and are the antisymmetric field tensors for and , respectively. It is known that the inclusion of nonlinear terms is essential to reproduce the properties of nuclei quantitatively and provide a reasonable value for the incompressibility, while the nonlinear term is added in order to reproduce the density dependence of the vector part of the nucleon self-energy obtained in the relativistic Brueckner Hartree–Fock (RBHF) theory (Sugahara & Toki, 1994a). We adopt the parameter set TM1 listed in Table 2, which was determined in Sugahara & Toki (1994a) by fitting some ground-state properties of nuclei including unstable ones. With the TM1 parameter set, the nuclear matter saturation density is fm, the binding energy per nucleon is MeV, the symmetry energy is MeV, and the incompressibility is MeV. The RMF theory with the TM1 parameter set provides an excellent description of nuclear matter and finite nuclei (Sugahara & Toki, 1994a), and it is also shown to agree satisfactorily with experimental data in studies of nuclei with deformed configurations (Hirata et al., 1996). For the parameters of hyperons, we use the experimental mass value MeV (Amsler et al., 2008). Concerning the coupling constants between mesons and hyperons, we take based on the naive quark model and determined by fitting experimental binding energies of single- hypernuclei (Shen et al., 2006), which produce an attractive potential of in nuclear matter at saturation density to be around MeV. It is known that the inclusion of tensor coupling between and is important to produce small spin-orbit splittings of single- hypernuclei, but it does not contribute to homogeneous matter. The hyperon is a charge neutral and isoscalar particle, so that it does not couple to the meson. It is shown that these parameters can reproduce well the experimental data for both single- and double- hypernuclei (Shen et al., 2006).

Starting with the Lagrangian (1), we derive a set of Euler–Lagrange equations. We employ the RMF approximation as described in Serot & Walecka (1986), where the meson fields are treated as classical fields and the field operators are replaced by their expectation values. For homogeneous matter, the non-vanishing expectation values of meson fields are , , and . The equations of motion for the meson fields in homogeneous matter have the following form:

 σ = −gσm2σ⟨¯ψψ⟩−gΛσm2σ⟨¯ψΛψΛ⟩−1m2σ(g2σ2+g3σ3), (2) ω = gωm2ω⟨¯ψγ0ψ⟩+gΛωm2ω⟨¯ψΛγ0ψΛ⟩−1m2ωc3ω3, (3) ρ = gρm2ρ⟨¯ψτ3γ0ψ⟩. (4)

The stationary Dirac equations for nucleons and hyperons are given by

 (−iαk∇k+βM∗N+gωω+gρτ3ρ)ψsN=εsNψsN, (5) (−iαk∇k+βM∗Λ+gΛωω)ψsΛ=εsΛψsΛ, (6)

where stands for the nucleons ( or ). and are the effective nucleon mass and effective mass, respectively. denotes the index of eigenstates, while and are the single-particle energies.

In homogeneous matter, baryons occupy single-particle states with the occupation probability (, , or ). At zero temperature, under the Fermi surface, while above the Fermi surface. For finite temperature, the occupation probability is given by the Fermi–Dirac distribution,

 fsi=11+exp[(εsi−μi)/T]=11+exp[(√k2+M∗i2−νi)/T], (7) fs¯i=11+exp[(−εs¯i+μi)/T]=11+exp[(√k2+M∗i2+νi)/T], (8)

where and denote the particle and antiparticle, respectively. and are the single-particle energies. The relation between the chemical potential and the kinetic part of the chemical potential is given by

 μp = νp+gωω+gρρ, (9) μn = νn+gωω−gρρ, (10) μΛ = νΛ+gΛωω. (11)

The chemical potential is related to the baryon number density as

 ni=1π2∫∞0dkk2(fki−fk¯i), (12)

where the quantum number is replaced by the momentum when we do the integration in the momentum space instead of summing over the eigenstates. We denote as the total baryon number density and as the proton fraction in homogeneous matter. The coupled equations are solved at fixed and . At zero temperature, hyperons appear only at high density when the equilibrium condition could be satisfied. For finite temperature, a small number of hyperons may exist at low density with , and the fraction increases rapidly at high density. The thermodynamic quantities of homogeneous matter have been derived in Serot & Walecka (1986)Shen et al. (1998a, b), and Shen (2002), so we simply write the expressions here. The energy density of nuclear matter including hyperons is given by

 ϵ = ∑i=p,n,Λ1π2∫∞0dkk2√k2+M∗i2(fki+fk¯i) (13) +12m2σσ2+13g2σ3+14g3σ4+12m2ωω2+34c3ω4+12m2ρρ2,

the pressure is given by

 p = ∑i=p,n,Λ13π2∫∞0dkk2k2√k2+M∗i2(fki+fk¯i) (14) −12m2σσ2−13g2σ3−14g3σ4+12m2ωω2+14c3ω4+12m2ρρ2,

and the entropy density is given by

 s =∑i=p,n,Λ1π2∫∞0dkk2 [−fkilnfki−(1−fki)ln(1−fki) (15) −fk¯ilnfk¯i−(1−fk¯i)ln(1−fk¯i)].

### 2.2 Thomas–Fermi approximation

In the low-temperature and low-density region, heavy nuclei may be formed in order to lower the free energy. We adopt the Thomas–Fermi approximation in combination with assumed nucleon distribution functions and a free energy minimization to describe the non-uniform matter based on the work by Oyamatsu (1993). In this study, we take into account the contribution from hyperons only when the fraction is larger than . In the region where the heavy nuclei are formed, is quite small, therefore we neglect the contribution from hyperons in the Thomas–Fermi calculation. The non-uniform matter is modeled as a mixture of a single species of heavy nuclei, alpha particles, and free nucleons that exist outside of nuclei, while the leptons can be treated as uniform non-interacting particles separately. For the system with a fixed proton fraction, the leptons play no role in the free energy minimization. Hence we mainly pay attention to the baryon contribution in this study.

We assume that each heavy spherical nucleus is located in the center of a charge-neutral cell consisting of a vapor of neutrons, protons, and alpha-particles. The nuclei form a body-centered-cubic (BCC) lattice to minimize the Coulomb lattice energy. It is useful to introduce the Wigner–Seitz cell to simplify the energy of a unit cell. The Wigner–Seitz cell is a sphere whose volume is the same as the unit cell in the BCC lattice. The lattice constant is defined as the cube root of the cell volume, , where and are the baryon number per cell and the average baryon number density, respectively. We define the baryon mass density as with being the atomic mass unit (Amsler et al., 2008). We calculate the Coulomb energy using the Wigner–Seitz approximation and adding an energy correction for the BCC lattice (Oyamatsu, 1993). This energy correction is negligible unless the nuclear size is comparable to the cell size.

We assume the nucleon distribution function ( or ) in the Wigner–Seitz cell as

 ni(r)=⎧⎪ ⎪⎨⎪ ⎪⎩(nini−nouti)[1−(rRi)ti]3+nouti,0≤r≤Ri,nouti,Ri≤r≤Rcell, (16)

where represents the distance from the center of the nucleus and is the radius of the Wigner–Seitz cell defined by . The density parameters and are the densities at and , respectively. The parameters and determine the boundary and the relative surface thickness of the nucleus. For the distribution function of alpha-particle , which should decrease as approaches the center of the nucleus, we assume

 (17)

which could give and . Here we use the same parameters and for both proton and alpha-particle distribution functions in order to avoid the presence of too many parameters in the minimization procedure. The parameters and may be somewhat different from and due to the additional neutrons forming a neutron skin in the surface region. For a system with fixed temperature , proton fraction , and baryon mass density , there are eight independent parameters among the ten variables, , , , , , , , , , and . The thermodynamically favorable state is the one that minimizes the free energy density with respect to these eight independent parameters. In principle, the resulting nucleon distribution in the Wigner–Seitz cell would depend on the form of the parameterization. It is also possible to determine the nucleon distribution by a self-consistent Thomas–Fermi method without any form of parameterization (Sil et al., 2001; Shen et al., 2010b). We have compared, in Figures 1 and 2 of Shen et al. (2010b), the results obtained by the self-consistent Thomas–Fermi method with those using the parameterization of Equation (16), and found that they were in good agreement with each other for the cases considered. Therefore, Equation (16) is considered to be a reasonable form of the nucleon distribution in the Wigner–Seitz cell.

In this model, the free energy density contributed from baryons is given by

 f=Fcell/a3=(Ecell−TScell)/a3, (18)

where the free energy per cell can be written as

 Fcell=(Ebulk+Es+EC)−TScell=Fbulk+Es+EC. (19)

The bulk energy , entropy , and free energy are calculated by

 Ebulk = ∫cellϵ(nn(r),np(r),nα(r))d3r, (20) Scell = (21) Fbulk = (22)

Here , , and are the local energy density, entropy density, and free energy density at the radius , where the system can be considered as a mixed uniform matter of neutrons, protons, and alpha-particles. These local densities are the sum of the contributions from nucleons and alpha particles. We use the RMF theory described in Section 2.1 to calculate the nucleon contribution, while the alpha-particles are treated as an ideal Boltzmann gas. In general, the number density of alpha-particles is quite small, and therefore the ideal-gas approximation is considered to be a reasonable approximation for alpha-particles. We note that other treatments for alpha-particles have been developed and used in nuclear astrophysics (Sumiyoshi & Röpke, 2008; Horowitz & Schwenk, 2006). The free energy density of alpha-particles in the ideal-gas approximation is given by

 fα(nα)=−Tnα[ln(8nQ/nα)+1]+nα(4M−Bα), (23)

where is the number density of alpha-particles, and we have used the abbreviation . The alpha-particle binding energy MeV is taken from Lattimer & Swesty (1991). We have to take into account the volume of alpha-particle, otherwise the alpha-particle fraction would become a large number at high density, where the alpha-particle should actually disappear. When we take into account the volume excluded by alpha-particles, the free energy densities of nucleons and alpha-particles are given by

 fN(nn,np) = (1−u)fN(~nn,~np), (24) fα(nα) = (1−u)fα(~nα), (25)

where is the fraction of space occupied by alpha-particles with the effective volume of alpha-particle taken from Lattimer & Swesty (1991). We denote the effective number density of neutrons, protons, or alpha-particles as (, , or ). The inclusion of the volume excluded by alpha-particles has negligible effect in the low-density region, whereas it is necessary for the calculation at high density.

As for the surface energy term due to the inhomogeneity of the nucleon distribution, we take the simple form

 Es=∫cellF0∣∇(nn(r)+np(r))∣2d3r. (26)

The parameter is determined by performing the Thomas–Fermi calculation for finite nuclei so as to reproduce the gross properties of nuclear masses, charge radii, and the beta stability line as described in the Appendix of Oyamatsu (1993).

The Coulomb energy per cell is calculated using the Wigner–Seitz approximation with an added correction term for the BCC lattice (Oyamatsu, 1993)

 EC=12∫celle[np(r)+2nα(r)−ne]ϕ(r)d3r+ΔEC, (27)

where represents the electrostatic potential calculated in the Wigner–Seitz approximation, is the electron number density of a uniform electron gas (), and is the correction term for the BCC lattice, which is approximated as

 ΔEC=CBCC(Znone)2a. (28)

Here is the lattice constant, is taken from Oyamatsu (1993), and is the non-uniform part of the charge number per cell given by

 Znon=∫Rp0(ninp−noutp−2noutα)[1−(rRp)tp]34πr2dr. (29)

Because of the long-range nature of the Coulomb interaction, is dependent on the lattice type. This dependence has been extensively discussed in Oyamatsu (1993). The system prefers the BCC lattice because it gives the lowest Coulomb energy. In general, the Coulomb energy is dependent on the temperature as discussed in Bravo & García-Senz (1999) and Potekhin & Chabrier (2010). The dependence of in Equation (27) is contained in the particle distributions. We assume that Equation (28), which was derived at zero temperature in Oyamatsu (1993), remains valid at finite temperature.

Since we assume the lattice of nuclei with the Wigner–Seitz approximation, we do not include a contribution from the translational energy of heavy nuclei. This contribution is small in general and does not affect the general behavior of the EOS. It may be noticeable only within the limited region of temperature, where nuclei behave as gas without being dissociated into nucleons. We note that this is different from the treatment by Lattimer & Swesty (1991), who included this term as a minor contribution.

## 3 Results

In this work, we construct the EOS tables covering a wide range of temperature , proton fraction , and baryon mass density for the use of core-collapse supernova simulations. We present two sets of EOS tables, namely EOS2 and EOS3. EOS2 takes into account only the nucleon degree of freedom, while EOS3 includes additional contributions from hyperons. In comparison with the earlier version (EOS1) described in Shen et al. (1998b), several improvements are made in EOS2 and EOS3 according to the requirements of the users. We largely increase the number of points, and adopt a linear grid in EOS2 and EOS3 instead of the logarithmic grid used in EOS1. On the other hand, the numerical methods are improved to allow the calculation with equal grid spacing for , while it is only approximately equal at high density in EOS1. For a detailed comparison between the EOS tables discussed in this paper, one can see Table 1 in Section 1. In principle, the matter at extremely high temperatures and densities is beyond the applicability of the RMF theory, but we still include the results in these exotic regions since they are sometimes necessary in astrophysical simulations.

### 3.1 Properties of matter without hyperons

In EOS2, we present results of matter without the inclusion of hyperons. For each , , and , we determine the thermodynamically favorable state that has the lowest free energy in the present model. We perform the free energy minimization for both non-uniform matter and uniform matter. Here the phase of heavy nuclei formed together with free nucleons and alpha-particles is referred to as non-uniform matter, while the phase of nucleons mixed with alpha-particles without heavy nuclei is referred to as uniform matter. For non-uniform matter, the minimization procedure is realized by using the Thomas–Fermi method which includes eight independent parameters as described in Section 2.2. For uniform matter, we perform the minimization with respect to converting two protons and two neutrons into an alpha-particle, in which there is only one independent parameter. By comparing the free energies of non-uniform matter and uniform matter, we determine the most favorable state and estimate the phase transition between non-uniform matter and uniform matter.

We first discuss the phase diagram of nuclear matter at finite temperature. It is known that the density of the phase transition between uniform matter and non-uniform matter depends on both and . The non-uniform matter phase can exist only in the low-temperature region ( MeV). In Figure 1, we show the phase diagram in the plane for , , and . The shaded region corresponds to the non-uniform matter phase where heavy nuclei are formed. The dashed line is the boundary where the alpha-particle fraction changes between and . It is shown that heavy nuclei can exist in the medium-density and low-temperature region. The phase of nuclear matter at low density is a homogeneous nucleon gas with a small fraction of alpha-particles, the heavy nuclei are formed at some medium densities where the system can lower the free energy by forming heavy nuclei, and it becomes uniform matter as the density increases beyond . It is seen that the starting density of the non-uniform matter phase depends on strongly, while the ending density is nearly independent of . As the temperature increases, the density range of the non-uniform matter phase becomes narrower, and it disappears completely for MeV. In Figure 2, we show the phase diagram in the plane for , , and MeV. The shaded region corresponds to the non-uniform matter phase, while the dashed line is the boundary between and . It is shown that the dependence of the boundary on is relatively weak except at very small values of . In the case of MeV (middle panel), the non-uniform matter phase disappears at lower because it is difficult to form heavy nuclei with smaller values of . The alpha-particles still exist at MeV, and reaches to be more than at some medium densities for as shown in the top panel of Figure 2. We note that the phase diagram of nuclear matter at zero temperature has been discussed in Shen et al. (1998a, b).

In the non-uniform matter, nucleon distributions are determined by minimizing the free energy density with respect to the independent parameters in the Thomas–Fermi approximation. The heavy nuclei are assumed to form a BCC lattice in order to minimize the Coulomb lattice energy. In Figure 3, we show the nucleon distributions along the straight line joining the centers of the nearest nuclei in the BCC lattice for the case of MeV and . It is found that the nuclei become heavier and get closer with each other as the density increases. In principle, there exist free nucleons and alpha-particles outside heavy nuclei at finite temperature, but their densities are too small to be observed in Figure 3. We show in Figure 4 the same quantities as in Figure 3 but for the case of MeV and . We note that the starting density of the non-uniform matter phase in this case is , so the heavy nucleus does not exist at for MeV which is different from the case of MeV as shown in the bottom panel of Figure 3. Comparing with the top and middle panels of Figure 3, it is seen that there are much more free nucleons and alpha-particles outside nuclei, while the nucleons inside nuclei get less. This is because the role of entropy becomes more important at higher temperature and the free energy can be lowered if the nucleons are freed from nuclei. In Figure 5, we plot the nuclear mass number and charge number as a function of the baryon mass density for at MeV and MeV. It is shown that and have relatively weak dependence on at lower density and they increase rapidly just before the phase transition at . For the same and , the values of and at MeV are much smaller than those at MeV. This is because more nucleons are freed from nuclei at higher temperature, and it is eventually impossible to form heavy nuclei for MeV in the present model.

In Figure 6, we show the fraction of neutrons, protons, alpha-particles, and heavy nuclei as a function of the baryon mass density for at , , and MeV. At low density, the matter is a uniform gas of neutrons and protons with a small fraction of alpha-particles. The alpha-particle fraction increases with increasing , but the formation of heavy nuclei at low temperatures causes a rapid drop of , , and , which is due to the fact that heavy nuclei use up most of the nucleons in non-uniform matter. When the density increases beyond , the heavy nuclei dissolve and the matter becomes uniform. The alpha-particles may exist up to where the volume excluded by alpha-particles plays an important role that it is unfavorable to have alpha-particles in the uniform matter at such high density. For MeV, the heavy nuclei cannot be formed, but there are finite values of , especially at medium densities as shown in the top panel of Figure 6. The alpha-particle fraction decreases with increasing temperature, and we find that at MeV is of the order of at some medium densities. The alpha-particle fraction may be significantly affected if the alpha-particle binding energy is dependent on the density and temperature as discussed in Röpke et al. (2005). For simplicity, we neglect this dependence and take MeV in the present model. Since we treat the uniform matter and non-uniform matter consistently using the same RMF theory, all the resulting thermodynamic quantities are consistent and smooth in the whole range. We will discuss the thermodynamic quantities in EOS2 and compare with those in EOS3 in the next section.

### 3.2 Properties of matter with the inclusion of Λ hyperons

In this section, we discuss results of matter with the inclusion of hyperons given in EOS3. It is found that the contribution from hyperons is negligible in the low-temperature and low-density region. In fact, at zero temperature hyperons appear only at high density when the equilibrium condition could be satisfied. At low temperature, such as MeV, the fraction is smaller than at densities below normal nuclear matter density. For simplicity, we take into account the contribution from hyperons only when is larger than . In the non-uniform matter phase, is quite small, therefore we neglect the contribution from hyperons in the Thomas–Fermi calculation.

In Figure 7, we show the fraction (, , , , or heavy nuclei ) as a function of for at , , and MeV. For lower temperatures, such as MeV (bottom panel) and MeV (middle panel), there is a significant fraction of hyperons only at high density. It is shown that increases with increasing , which causes a decrease of . We note that , which is equal to in the uniform matter at high density, has been fixed to be in this figure. For MeV (top panel), is of the order of at low density, and increases rapidly at high density. Comparing with the top panel of Figure 6, it is seen that the inclusion of hyperons does not affect and significantly. We find the contribution from hyperons increases with increasing temperature. At MeV, is about 12% at low density for the case of . On the other hand, decreases with increasing at fixed and , since there are less neutrons at higher to realize the equilibrium condition .

We now discuss the thermodynamic quantities in EOS3 and compare with those in EOS2. Here we mainly discuss their properties at high density where there are noticeable differences between the results with and without hyperons. As for the behavior of thermodynamic quantities at low density, one can refer to our earlier work (Shen et al., 1998a, b). In Figure 8, we show the free energy per baryon as a function of the baryon mass density with and at , , and MeV. The results with hyperons given in EOS3 are shown by solid lines, while those without hyperons given in EOS2 are displayed by dashed lines. It is found that the inclusion of hyperons can lower the free energy and this effect increases with increasing . However, this effect decreases with increasing as shown in Figure 8, which is due to the fact that decreases with increasing . We show in Figure 9 the pressure as a function of with and at , , and MeV. The pressure is calculated from the derivative of the free energy as described in Appendix A. Therefore, the effect of hyperons on the pressure is similar to the one observed in Figure 8. It is obvious that the inclusion of hyperons tends to soften the EOS at high density. In Figure 10, we show the entropy per baryon as a function of with and at , , and MeV. At MeV (bottom panel) it is hard to see the difference between the results with and without hyperons, while at MeV (middle panel) there are small differences at high density. For the case of MeV (top panel), the effect of hyperons can be seen in the whole range of density, since reaches () at low density for () at MeV. In general, the inclusion of hyperons tends to increase the entropy. In Shen et al. (1998a, b), we have discussed the effect of the formation of nuclei on the entropy, which has a strong dependence. The behavior of at in the middle and bottom panels of Figure 10 is due to the formation of heavy nuclei in non-uniform matter.

For neutron star matter at zero temperature, the inclusion of hyperons leads to a softening of the EOS of neutron star matter and thereby a corresponding reduction in the maximum mass of neutron stars. We use EOS3 to calculate the neutron star properties and find that the maximum mass of neutron stars is about 1.75 , whereas the value for EOS1 and EOS2 is 2.18 . According to the recent measurement of PSR J1614-2230 (Demorest et al. (2010)), EOS3 seems to be too soft due to the inclusion of hyperons, while EOS1 and EOS2 are compatible with the observation of PSR J1614-2230. This is a common difficulty for EOSs with the inclusion of hyperons. So far, there are large uncertainties in the properties of matter at high density, which are crucial for determining the maximum mass of neutron stars.

## 4 Summary

In this paper, we have presented two sets of the EOS tables (EOS2 and EOS3) covering a wide range of temperature , proton fraction , and baryon mass density for the use of core-collapse supernova simulations. The difference between EOS2 and EOS3 is that only the nucleon degree of freedom is taken into account in EOS2, while EOS3 includes additional contributions from hyperons. In comparison with the earlier version (EOS1) described in Shen et al. (1998b), several improvements have been made in EOS2 and EOS3 according to the requirements of the users. We have largely increased the number of points, and adopted a linear grid in EOS2 and EOS3 instead of the logarithmic grid used in EOS1. In addition, we have performed the calculation with equal grid spacing in the whole range of density, while it is only approximately equal at high density in EOS1. We have presented a detailed comparison between these EOSs in Table 1.

We have employed the RMF theory with nonlinear and terms, which can provide an excellent description of nuclear matter and finite nuclei including unstable ones. The Thomas–Fermi approximation in combination with assumed nucleon distribution functions and a free energy minimization has been adopted to describe the non-uniform matter that is modeled as a mixture of a single species of heavy nuclei, alpha particles, and free nucleons outside of nuclei. The RMF results have been taken as input in the Thomas–Fermi calculation, so the treatments of non-uniform matter and uniform matter in this EOS are sufficient to obtain the table in a consistent manner. It would be preferable to treat the mixture of nuclei as recently done in Hempel & Schaffner-Bielich (2010)Furusawa et al. (2011), and Blinnikov et al. (2011) for the detailed treatment of electron captures on nuclei in supernova core. However, it is beyond the scope of the current update of the Shen EOS table, which has been routinely used in astrophysical simulations.

We have included the contribution from hyperons in EOS3, when the fraction is larger than . It is based on the consideration that the hyperon is most likely to occur in dense matter among all possible non-nucleonic degrees of freedom because it is the lightest hyperon with an attractive potential in nuclear matter. The potential depth of in nuclear matter is estimated to be around MeV from the experimental binding energies of single- hypernuclei. Several recent observations of double- hypernuclei suggest that the effective interaction should be weakly attractive. The RMF theory with nonlinear and terms has been extended to include hyperons, and it can provide a reasonable description of single- and double- hypernuclei (Shen et al., 2006). We have not included contributions from other hyperons, such as and , due to their relatively high threshold densities and lack of available experimental data. In EOS3, we have performed a consistent calculation including hyperons for the entire table, whereas the EOS tables of high density matter were connected with EOS1 at low density in the simple procedure described in Section 2.3 of Ishizuka et al. (2008), so EOS3 is considered to be constructed in a consistent manner for the inclusion of hyperons. We have examined the effect of hyperons on the properties of dense matter. The contribution from hyperons is negligible in the low-temperature and low-density region, whereas it tends to soften the EOS at high density.

In principle, the matter at extremely high temperatures and densities is beyond the applicability of the RMF theory, but we still include the results in these exotic regions since they are sometimes necessary in astrophysical simulations. It will continue to be a challenge for nuclear physics to provide realistic EOS, which should be supported by microscopic theory and available experimental data, for use in astrophysical studies.

We thank C. D. Ott and T. Fischer for helpful suggestions and fruitful discussions. K.S. expresses his thanks to K. Nakazato, A. Ohnishi, H. Suzuki, and S. Yamada for practical discussions on the development of the EOS tables for simulations. H.S. and K.S. thank the organizers of the MICRA2011 workshop hosted by the Perimeter Institute. This work was partially supported by the National Natural Science Foundation of China (grant nos. 10675064 and 11075082), the Grant-in-Aid for Scientific Research on Innovative Areas (nos. 20105004 and 20105005), and the Grant-in-Aid for the Scientific Research (no. 22540296) from the Ministry of Education, Culture, Sports, Science and Technology (MEXT) of Japan. This work for numerical simulations of core-collapse supernovae is partially supported by the HPCI Strategic Program of MEXT in Japan, which assists K.S. to use the supercomputers at Yukawa Institute for Theoretical Physics (YITP) in Kyoto University, Research Center for Nuclear Physics (RCNP) in Osaka University, the University of Tokyo, Japan Atomic Energy Agency (JAEA) and High Energy Accelerator Research Organization (KEK).

## Appendix A Physical quantities in the EOS tables

The EOS tables are available on the Web at
http://physics.nankai.edu.cn/grzy/shenhong/EOS/index.html,
,
http://user.numazu-ct.ac.jp/sumi/eos/index.html.
The table under the name “.tab” is the main EOS table, while “.t00” and “.yp0” are those for and , respectively. EOS2 and EOS3 are presented in electronic tables, Tables 3–8, in this paper. We present the main EOS table of EOS2 (EOS3) in Table 3 (Table 6), which is 149 MB (167 MB) in size. Table 4 (Table 7) is the one of EOS2 (EOS3) at which is 1.6 MB (1.8 MB), while Table 5 (Table 8) is the one for which is 2.3 MB (2.6 MB). The tables are written in the order of increasing . In the tables on the Web, the values of and (in MeV) are given at the beginning of each block, and the blocks with different are divided by the string of characters “cccccccccccc”. In Tables 3–8 of this paper, and are set in columns 1 and 2. We note that the entry for is set to in the tables for the case of .

For each , we present the results in the order of increasing and . The quantities in one line of Tables 3–8 are defined as follows.

• 1. Logarithm of temperature: [MeV].

• 2. Temperature: [MeV].

• 3. Logarithm of baryon mass density: [].

• 4. Baryon number density: [].
The baryon number density is related to the baryon mass density as with MeV being the atomic mass unit taken from Amsler et al. (2008).

• 5. Proton fraction: .
The proton fraction of uniform matter is defined by

 Yp=np+2nαnB=np+2nαnp+nn+nΛ+4nα, (A1)

where , , , and are the number density of protons, neutrons, hyperons, and alpha-particles, respectively. is the total baryon number density. For non-uniform matter case, is the average proton fraction defined by

 Yp=NpNB, (A2)

where and are the proton and baryon numbers per cell given by

 Np = ∫cell[np(r)+2nα(r)]d3r, (A3) NB = ∫cell[nn(r)+np(r)+4nα(r)]d3r. (A4)

Here, and are the proton and neutron distributions given by Equation (16), and is the alpha-particle distribution given by Equation (17). Because the fraction is very small in the non-uniform matter phase, we neglect the contribution from hyperons in this case.

• 6. Free energy per baryon: [MeV].
The free energy per baryon is defined relative to the free nucleon mass MeV in the TM1 parameter set as

 F=fnB−M. (A5)
• 7. Internal energy per baryon: [MeV].
The internal energy per baryon is defined relative to the atomic mass unit MeV as

 Eint=ϵnB−mu. (A6)
• 8. Entropy per baryon: [].
The entropy per baryon is related to the entropy density via

 S=snB. (A7)
• 9. Mass number of the heavy nucleus: .
The mass number of the heavy nucleus is defined by

 A=∫RA0[nn(r)+np(r)]4πr2dr, (A8)

where is the maximum of and , which is considered as the boundary of the heavy nucleus.

• 10. Charge number of the heavy nucleus: .
The charge number of the heavy nucleus is defined by

 Z=∫RA0np(r)4πr2dr. (A9)
• 11. Effective nucleon mass: [MeV].
The effective nucleon mass is obtained in the RMF theory for uniform matter. In the non-uniform matter phase, the effective nucleon mass is a function of space due to inhomogeneity of the nucleon distribution, so it is meaningless to list the effective nucleon mass for non-uniform matter. We replace the effective nucleon mass by the free nucleon mass in the non-uniform matter phase.

• 12. Free neutron fraction: .
The free neutron fraction is given by

 Xn=(noutnVout)/(nBVcell), (A10)

where is the cell volume, is the volume outside the nucleus, is the number density of free neutrons outside the nucleus, and is the average baryon number density.

• 13. Free proton fraction: .
The free proton fraction is given by

 Xp=(noutpVout)/(nBVcell), (A11)

where is the number density of free protons outside the nucleus.

• 14. Alpha-particle fraction: .
The alpha-particle fraction is defined by

 Xα=4Nα/(nBVcell), (A12)

where is the alpha-particle number per cell obtained by

 Nα=∫cellnα(r)d3r (A13)

and is the alpha-particle distribution given by Equation (17).

• 15. Heavy nucleus fraction: .
The heavy nucleus fraction is defined by

 XA=A/(nBVcell), (A14)

where is the mass number of the heavy nucleus as defined in Equation (A8).

• 16. Pressure: [].
The pressure is calculated through the thermodynamic relation

 p=[n2B(∂F/∂nB)]T,Yp. (A15)
• 17. Chemical potential of the neutron: [MeV].
The chemical potential of the neutron relative to the free nucleon mass is calculated through the thermodynamic relation

 μn=[∂(nBF)/∂nn+Λ]T,np, (A16)

where is the sum of the neutron and densities.

• 18. Chemical potential of the proton: [MeV].
The chemical potential of the proton relative to the free nucleon mass is calculated through the thermodynamic relation

 μp=[∂(nBF)/∂np]T,nn+Λ. (A17)
• 19. Effective mass: [MeV].
The effective mass is obtained in the RMF theory for uniform matter. We replace the effective mass by the free mass MeV when the hyperon is not taken into account.

• 20. fraction: .
The fraction is given by

 XΛ=nΛ/nB, (A18)

where is the number density of hyperons in the uniform matter phase. We note that is adopted in the non-uniform matter phase.

## Appendix B Checks on the EOS tables

We have done the following checks on the EOS tables.

• 1. Consistency of the fractions:

 Xp+Xn+XΛ+Xα+XA=1. (B1)
• 2. Consistency of the relation between , , and :

 F=Eint−TS+mu−M. (B2)
• 3. Consistency of the thermodynamic quantities:

 F=μn(1−Yp)+μpYp−pnB. (B3)

In general, these consistency relations can be satisfied within a few thousandths. The physical constants used in this study are taken from Amsler et al. (2008).