The Properties of Nuclear Matter

The microscopic and bulk properties of nuclear matter at zero and finite temperatures are studied in the frame of the Brueckner theory. The results for the symmetry energy are also obtained using different potentials. The calculations are based on realistic nucleon-nucleon interactions which reproduce the nucleon-nucleon phase shifts. These microscopic approaches are supplemented by a density-dependent contact interaction to achieve the empirical saturation property of symmetric nuclear matter. Special attention is paid to behavior of the effective mass in asymmetric nuclear matter. The nuclear symmetry potential at fixed nuclear density is also calculated and its value decreases with increasing the nucleon energy. The hot properties of nuclear matter are also calculated using T 2-approximation at low temperatures. Good agreement is obtained in comparison with previous works around the saturation point.


I. INTRODUCTION
One of the most fundamental problems in nuclear many-body theory is the attempt to evaluate the nuclear matter binding energy and saturation properties, starting from a realistic Nucleon-Nucleon (NN) interaction with no free parameters. In fact a lot of work has been done trying to solve this problem using different approaches and methods which are discussed in details by Müther and Polls (2000). An important ingredient of all these approaches is the consideration of the two-nucleon correlations which are induced by the strong short-range components of the NN interaction. In lowest-order Brueckner theory, the familiar Brueckner-Hartree-Fock (BHF) approach, is adopted to calculate the energy, the so-called Gmatrix for evaluating the energy in the Hartree-Fock approach. In the G-matrix one accounts for the particle-particle correlations which means the scattering of two nucleons from states which are occupied in the Slatter determinant describing the ground state, into unoccupied particle states above the Fermi surface (Frick et al., 2002;2004;Hassaneen and Müther, 2004).
The potentials we will employ here are the recent models of the Nijmegen group (Stoks et al., 1994), the Argonne V 18 potential (Wiringa et al., 1995) and the charge-dependent Bonn potential (CD-Bonn) (Machleidt et al., 1996). The recent versions of The Nijmegen group are Nijm-I, Nijm-II and Reid93 potentials. Although all these potentials predict almost identical phase shifts, their mathematical structure is quite different.
Most of the microscopic calculations have been addressed to study symmetric matter (Frick et al., 2002) and pure neutron matter (Frick and Müther, 2003; Science Publications PI Dieperink et al., 2003). The study of asymmetric nuclear matter is technically more involved and only few Brueckner-Hartree-Fock (BHF) calculations are available Zuo et al., 1999;Vidana and Bombaci, 2002). The BHF approximation includes the self-consistent procedure of determining the single-particle auxiliary potential, as first devised by Brueckner and Gammel (1958), which is an essential ingredient of the method. Different approaches have been used to study the EoS of asymmetric nuclear matter including Dirac-Brueckner-Hartree-Fock (DBHF) calculations (Müther et al., 1987;Alonso and Sammarruca, 2003), Brueckner-Hartree-Fock (BHF) approximation to Brueckner-Bethe-Goldstone (BBG) calculations (Bombaci and Lombardo, 1991;Baldo and Ferreira, 1999) and variational methods (Wiringa et al., 1988;Akmal and Pandharipande, 1997). Besides these microscopic approaches, effective theories such as Relativistic Mean Field (RMF) theory (Sugahara and Toki, 1994) and non-relativistic effective interactions (Stone et al., 2002; have also been used extensively to study the EoS and mean field properties of the asymmetric nuclear matter. As it is well known, the BHF approximation largely violates the Hugenholtz-Van Hove (HVH) theorem (Hugenholtz and Hove, 1958), which basically measures the consistency of a given order of approximation in a perturbative approach. In symmetric nuclear matter, the inclusion of the so-called hole-hole (hh) contribution greatly improves the fulfillment of the HVH theorem (Gad, 2004). We use realistic NN forces and operate within SCGF framework. It is well known that the selfconsistent BHF approach does not reproduce the correct saturation point of nuclear matter with only the inclusion of the two-body interaction (Bozek and Czerski, 2001;Bozek, 2002). But our attention is mainly focused on how nuclear matter properties change in terms of the asymmetry ratio and some caution has to be taken whenever saturation properties are involved. In addition, it gives a simple microscopic justification of the empirical laws governing asymmetric nuclear matter.

In the Present Report
In order to establish the importance of the hh term in the calculation of EoS for asymmetric nuclear matter our aim is to extend the BHF approach which ignores the hh term to SCGF approach, which includes the hh term. It has been shown, in the case of pure neutron matter (Zuo et al., 1998) and also symmetric nuclear matter (Frick et al., 2002;Zuo et al., 1998) that the new terms give a large contribution to single-particle properties like the mean field and the nucleon effective mass. We will refer to the present approach to compute nuclear single-particle properties as SCGF approximation (Frick et al., 2002;Hassaneen and Müther, 2004).
The nuclear matter symmetry energy, which is defined as the difference in energy per nucleon between the pure neutron matter and the symmetric nuclear matter, is an important quantity that determines the properties of objects such as the atomic nucleus and the neutron star (Li et al., 2008). The study of symmetry energy and its dependence on nuclear density and temperature is currently a subject of great interest (Baran et al., 2005). Theoretically, the symmetry energy can be determined from microscopic calculations such as the Self-Consistent Green Function (SCGF) and the Dirac-Brueckner-Hartree-Fock (DBHF) calculations, or the phenomenological calculations such as the Skyrme Hartree-Fock (SHF) and the Relativistic Mean Field (RMF) calculations Li et al., 2008;Gad and Hassaneen, 2007;Gögelein et al., 2009). These calculations currently predict wide range of symmetry energies for densities below and above normal nuclear density, ρ 0 = 0:16 fm −3 . Also, the symmetry energy and its relation with the chemical potential have been studied.
Also, the properties of asymmetric nuclear matter are derived from various many-body approaches. This includes phenomenological ones like the Skyrme Hartree-Fock and relativistic mean field approaches, which are adjusted to fit properties of nuclei, as well as more microscopic attempts like the Brueckner-Hartree-Fock approximation, a self-consistent Greens function method and the so-called V lowk approach. These microscopic approaches are supplemented by a densitydependent contact interaction to achieve the empirical saturation property of symmetric nuclear matter. The predictions of the isovector component of the effective mass in neutron-rich matter, the symmetry potential and symmetry energy are discussed.
The one-body potentials for protons and neutrons are obtained from the self-consistent Green-function calculations of asymmetric nuclear matter, in particular their dependence on the degree of proton/neutron asymmetry. Results of the binding energy per nucleon as a function of the density and asymmetry parameter are presented for the self-consistent Green function approach using the CD-Bonn potential. The nuclear symmetry potential at fixed nuclear density is also calculated and Science Publications PI its value decreases with increasing the nucleon energy. The isoscalar proton/neutron effective mass splitting in neutron-rich matter has been studied.
Recently, Li et al. (2006) have studied the saturation properties of nuclear matter within the Brueckner-Hartree-Fock approach using continuous single particle energies and employing the most recent accurate nucleon-nucleon potentials. They found that their results confirm the concept of "Coester line" or "Coester band", i.e., density and energy of the various saturation points being strongly correlated, yielding either a too large saturation density or a too small binding energy.
The many-body method we will employ in deriving the EoS of both symmetric and pure nuclear matter is a rather simple one i.e., the non-relativistic BHF method with a conventional and continuous single particle spectrum using different modern NN potentials.
The results in the present work which come out by approximating the single particle self-consistent potential with a parabolic form.

Brueckner-Hartree-Fock for Symmetric Nuclear Matter
In the BHF approximation, the nuclear matter total energy E A is obtained from the Brueckner G-matrix, G(ω), according to the Equation (1): with |k 1 k 2 〉 a = |k2k1〉, i.e., the subscript a indicates antisymmetrization of the matrix elements. Here k F is the Fermi momentum, the summation over the momenta k i include spin and isospin variables. The single particle energies e k , appearing in the entry energy of the Gmatrix, are given by Equation (2): where, the single particle potential U(k) is determined by the self-consistent Equation (3): The self-consistency is coupled with the integral equation for the G-matrix, i.e., in the BHF approach G(ω) is obtained by solving the Bethe-Goldstone equation: where, Θ F (k) = 1 defining the step function for k<k F and is zero otherwise and ω denotes the starting energy. The product Q(k, k') = (1-Θ F (k))(1-Θ F (k')), appearing in the kernel of Equation (4), enforces the scattered momenta to lie outside the Fermi sphere and it is commonly referred to as the "Pauli operator". In the case of the angle-average of Pauli operator this energy is given as Equation (5), (Haftel and Tabakinc, 1970): If one assumes that the potential U(k), or equivalently the single particle energy e(k), has approximately a quadratic form: where, e 0 is the zero point energy. Then one can calculate the potential, at each iteration step, in few points only and interpolate the obtained values with a parabola. The approximation of Equation (6) is usually called the effective mass approximation, since then the spectrum has the same shape as the free one but with an effective mass m*. From Equation (2) and (6) the effective mass m* can be evaluated from the slope of U(k) at the Fermi momentum Equation (7) (Mahaux and Sartor, 1991):

Brueckner-Hartree-Fock for Asymmetric Nuclear Matter
The self-energy of a nucleon with isospin i, momentum k and energy ω in asymmetric nuclear matter is defined in the BHF approximation by (Müther and Polls, 2000;Hassaneen and Müther, 2004): In this equation 0 j n (q) refers to the occupation probability of a free Fermi gas of protons (j = p) and neutrons (j = n) like in the mean-field or Hartree-Fock approach. This means that for asymmetric matter with a total density ρ = ρ p +ρ n this probability is defined by Equation (9): With Fermi momenta for protons (k Fp ) and neutrons (k Fn ).
The antisymmetrized G matrix elements in Equation (8) are obtained from a given NN interaction by solving the Bethe-Goldstone equation: The single-particle energies ε pi of the intermediate states should be the corresponding BHF single-particle energies which are defined in terms of the real part of the BHF self-energy of Equation (8) by Equation (11): with a starting energy parameter Ω = ω+ε qj in the Bethe-Goldstone Equation (10).

Self-Consistent Green's Function
One of the drawbacks of the BHF approximation is the fact that it does not provide results for the equation of state, which are consistent from the point of view of thermodynamics. As an example we mention that BHF results do not fulfill e.g., the Hugenholtz van Hove theorem. This is due to the fact that the BHF approximation does not consider the propagation of particle and hole states on equal footing. An extension of the BHF approximation, which obeys this symmetry is the Self-Consistent Green's Function (SCGF) method. During the last years techniques have been developed, which allow to evaluate the solution of the SCGF equations for microscopic NN interactions. Those calculation demonstrate that for the case of realistic NN interactions, the contribution of particle-particle ladders dominates the contribution of corresponding hole-hole propagation terms. This justifies the use of the BHF approximation and a procedure, which goes beyond BHF and accounts for hole-hole terms in a perturbative way (Frick et al., 2002;Grange et al., 1987). This leads to a modification of the self-energy in the BHF approximation by adding a hole-hole term of the form Equation (12): The quasi-particle energy for the extended selfenergy can be defined as Equation (13): Accordingly, the Fermi energy is obtained evaluating this definition at the Fermi momentum k = k Fi for protons and neutrons, respectively Equation (14): The spectral functions for hole and particle strength, where, the plus and minus sign on the left-hand side of this equation refers to the case of hole (h, ω<ε Fi ) and particle states (p, ω>ε Fi ), respectively. The hole strength represents the probability that a nucleon with isospin i, momentum k and energy ω can be removed from the ground state of the nuclear system with the removal energy ω, whereas the particle strength denotes the probability that such a nucleon can be added to the ground state of the system with A nucleons resulting in a state of the A+1 particle system which has an energy of ω Science Publications PI relative to the ground state of the A particle system. Hence the occupation probability is obtained by integrating the hole part of the spectral function Equation (16): Note that this yields values for the occupation probability, which ranges between values of 0 and 1 for all momenta k, leading to a partial depletion of the hole-states in the Fermi gas model (k<k F ) and partial occupations for states with momenta h>k F . A similar integral yields the mean energy for the distribution of the hole and particle strength, respectively Equation (17 and 18): Our self-consistent Green's function calculation is defined by identifying the single particle energy in the Bethe-Goldstone equation as well as in the 2h1p correction term in Equation (12 and 19): This definition leads to a single particle Greens function, which is defined for each momentum k by just one pole at ω = ε kτ . Hence, the total energy per nucleon is evaluated by Equation (20): In order to achieve saturation in nuclear matter one has to add three-body interaction terms or a densitydependent two-nucleon interaction. So, it is quite natural to supplement the effective interaction by a simple contact interaction, which we have chosen following the notation of the Skyrme interaction to be of the form: where, ρ is the matter density, t 0 , t 3 and δ are parameters. For a fixed value of δ (typically δ = 0.5) we have fitted t 0 and t 3 in such a way that a Hartree-Fock calculation using V lowk plus the contact term of Equation (21) yields the empirical saturation point for symmetric nuclear matter. The same parameterization of a contact term has been used to evaluate corrections to the self-energy of BHF and SCGF in such a way that also these calculations reproduce the saturation of symmetric nuclear matter. The many-body problem at finite temperatures has been considered by several authors within different approaches, such as the finite temperature Green's function method (Fetter and Walecka, 1971), the thermo field method (Henning, 1995), or the Bloch-De Domicis (BD) diagrammatic expansion (Bloch, 1958;Bloch and De Domicis, 1958). The latter, was developed soon after the Brueckner theory, represents the "natural" extension to finite temperature of the BBG expansion, to which it leads in the zero temperature limit. Baldo and Ferreira (1999) showed that the dominant terms in the BD expansion were those that correspond to the zero temperature of the Brueckner-Bethe-Goldstone (BBG) diagrams, where the temperature is introduced only through the Fermi-Dirac distribution Equation (22): Therefore, at the BHF level, finite temperature effects can be introduced in a very good approximation just replacing in the BGE (4): • the zero temperature Pauli operator Q = (1-θ 1 (k))(1θ 2 (k)) by the corresponding finite temperature one Q(T) = (1−f 1 )(1−f 2 ) • The single-particle energies e (k) by the temperature dependent ones e (k, T)), obtained from Equation (3) and (4) when θ (k) is replaced by f (k, T) In the present work, two simplifications are used to calculate the thermodynamic properties of nuclear matter. Firstly, the G-matrix calculation is performed at T = 0 MeV and using the continuous choice for U (k). Secondly, the internal energy of the system F→F/A, is computing by using the entropy of the free Fermi gas with effective mass m * , where the internal energy of nuclear mater is defined by: where, E→E/A is the total energy at T = 0, S T is the entropy of the system at temperature T. In addition thermal effects are treated in a low temperature limit of

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PI the internal energy. Starting from Equation (23), in the low temperature limit the energy and entropy behave as E = E T=0 + aT 2 and S T = 2aT, respectively, where a is the so-called level density parameter. Therefore, for the internal energy we have the following expression: With Equation (25): where, the level density parameter a is a function of the nucleon effective mass m * at T = 0 MeV with k = k F . By using Equation (24) the internal energy (Mansour et al., 1997) of the system at temperature T is defined by Equation (26): where m * is the effective mass of the nucleon at zero temperature with k = k F , defined in Equation (7). It should be pointed out that the same expressions are obtained for zero range forces (Barranco and Treiner, 1981). In fact they reflect a general property of the Landau theory of normal Fermi liquids.

The Single Particle Energy
In this section we present the results for the single particle energies which is calculating using Equation (2). More discussion can be read in (Hassaneen et al., 2011). Figure 1 shows the dependence of the single particle energy on the momentum k up to k fit = 1.6 k F for symmetric nuclear matter using the CD-Bonn potential (solid curve), the Argonne V 18 potential (dashed-double dot curve), the Nijm-I potential (dotted curve), the Nijm-II potential (dashed curve) and the Reid 93 potential (dashed-dot curve) at the normal saturation density ρ 0 = 0.16fm −3 in terms of Fermi momentum, k F = 1.333 fm −1 . Left panel for conventional choice, right panel for continuous choice. We observe that the results of all potentials are close to each other in the conventional choice and at high momentum after k = k F the results of all potentials come together, this means that the effect of the potential disappear at values above Fermi momentum k F . In the continuous choice we note that the CD-Bonn and Nijm-I (non-local) potentials are more attractive than the Argonne V 18 , the Nijm-II and the Reid 93 (local) potentials and the difference between the potentials continues even at high momentum k, this means that the effect of the potential continues at values above k F .
If we compare the results we note that, one finds that the single particle energies are more attractive in the continuous choice than those in the conventional choice. This reflects the fact that the effective interaction is more attractive between nucleons in the continuous choice than the conventional choice. From Fig. 1 one can also see that the BHF single particle energies have a simple parabolic shape as a function of the momentum for all the interactions. So, one uses a parametrization of the single particle energies in terms of an effective mass using Equation (7).
Finally we want to stress that, despite the parabolic approximation is not accurate (Baldo and Fiasconaro, 2000) and we use a not so large cutoff for the single particle momentum, we believe that the differences in the results for various NN interactions, obtained within the same approximation scheme, are sensible and meaningful.

The Nuclear Matter Binding Energy
We present the results of the non-relativistic BHF calculations in Fig. 2 obtained with different modern NN potentials. The energy per particle E A in MeV is plotted against the density ρ in terms of Fermi momentum k F in fm −1 , for symmetric nuclear matter using different potentials, the CD-Bonn potential (solid line), the three Nijmegen potentials, Nijm-I (short dashes), Nijm-II (double dot-dashed line) and Reid 93 (dot-dashed line) and the Argonne V 18 potential (dotted line). Left panel is for conventional choice and the right panel is for continuous choice. The solid points indicate the saturation points and the dashed box indicates the empirical saturation one. One observes from the figure that the binding energy per nucleon, first decreases with increasing k F , until it reaches the minimum (saturation) point then it increases with increasing the Fermi momentum k F . The continuous choice leads to an enhancement of correlation effects in the medium and tends to predict larger binding energies for nuclear matter than the conventional choice.

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It is found that our calculations lead to results for saturation points, which lie along a line (Coester line) shifted with respect to the phenomenological saturation point (ρ 0 = 0.16 fm −3 ; E A = -16MeV ). One can see that the continuous choice leads to an enhancement of correlation effects in the medium and tends to predict larger binding energies for nuclear matter than the conventional choice. In the continuous choice that line is close to the empirical data than the conventional choice. So, we can say that our results confirm the concept of a "line", density and energy of the various saturation points being strongly linearly correlated, where that be consistent with the results in (Li et al., 2006;Day, 1981). The saturation points for our results are presented in Table 1.
A very important source for the origin of the twobody correlations is the tensor force, which for example, describes the scattering of a proton-neutron pair, which originally is in a relative 3 S 1 state with momentum below k F , into a 3 D 1 state above the Fermi sea. A measure of the strength of the tensor force is expressed in term of the Dstate probability P D obtained for the deuteron (Day, 1981;Hjorth-Jensen et al., 1995). These D-state probabilities for the present potentials are listed in Table  1. We also observe from Table 1 that the continuous choice in the Nijm-II potential and Argonne V 18 potential obey approximately the correct Fermi momentum saturation point but at low binding energy per nucleon. The continuous choice in the Nijm-I potential obeys approximately the correct binding energy per nucleon but at high Fermi momentum. The CD-Bonn potential leads to strong over-binding and too high saturation density than the others, because it contains a weak tensor force. It looks that any increase of the nonlocality would improve the fitting of binding energy of nuclear matter, but shifts the saturation point to higher density and binding energy.
In Fig. 3, we plot, for comparison also, the energy per particle as a function of Fermi momentum k F using the continuous choice for the single particle auxiliary potential with the results obtained with the T-matrix and T-matrix +3BF method with CD-Bonn potential by Somua and Bozek (2008) and with BHF +3BF using both CD-Bonn and Argonne V 18 potentials by Baldo and Shaban (2008). There is another method can be used to enhance the present results if one goes beyond BHF approach.
In Fig. 4, the energy per particle E A is plotted against Fermi momentum k F , for pure neutron matter using different potentials. Left panel is for conventional choice, right panel is for continuous choice. We compare the results by CD-Bonn +3BF and V 18 +3BF. The pure neutron matter EoS is unbound with the energy per nucleon rising approximately monotonically with increasing the Fermi momentum, which is in agreement with most of the many-body calculations. We note that the differences between the potentials are small, because the main source of differences among the potentials is in the strength of the tensor force, which is mostly reflected in the (T = 0) 3 S 1 -3 D 1 coupled states. In pure neutron matter (T = 1), however, this partial wave does not contribute.
Only T=1 states contribute to the energy of pure neutron matter while both isospin states contribute to the energy of symmetric nuclear matter, if major T = 0 partial waves become increasingly repulsive at short distances. It is possible for the energy of symmetric nuclear matter to grow at a faster rate and eventually approach the neutron matter EoS. This is just what we observe in our model. In the presence of repulsive forces only, symmetric matter would be a more repulsive system than neutron matter (for the same k F ).

Symmetry Energy
The neutron matter EoS combined with that of symmetric nuclear matter provides us with information on the isospin effects (Zuo et al., 1999), in particular on the symmetry energy. The symmetry energy of nuclear matter is defined as a second derivative of energy per nucleon E A with respect to the asymmetry parameter α as follows Equation (27 and 28): where, we introduce the asymmetry parameter: Both ρ n and ρ p are the neutron and proton densities in Asymmetric Nuclear Matter (ANM) and ρ = ρ n + ρ p is the total density of asymmetric nuclear matter. It is well established (Gad and Hassaneen, 2007;Hassaneen and Gad, 2008;Bombaci and Lombardo, 1991) that the binding energy per nucleon E A fulfills the simple a 2 -law not only for a«1 as assumed in the empirical nuclear mass formula (Haustein, 1988), but also in the whole asymmetry range. The a 2 -law of the EoS of ANM at any isospin asymmetry leads to two important consequences.
First, it indicates that the EoS of ASM at any isospin asymmetry is determined completely by the EoS of SNM and the symmetry energy.   Second, the above a 2 -law implies that the difference of the neutron and proton chemical potentials in β-stable neutron star is determined by the symmetry energy in an explicit way: µ n -µ p = 4aE sym (Hassaneen and Gad, 2008) and thus the symmetry energy plays a crucial role in predicting the composition of neutron stars.
This enables us to calculate the symmetry energy E sym in terms of the difference between the binding energy of pure neutron matter E A (ρ,1) and that of symmetric nuclear matter E A (ρ,0), i.e., Equation (29): but one would refrain from applying it at very high density.
The results of our calculation for the symmetry energy as a function of baryonic density in terms of the Fermi momentum k F are depicted in Fig. 5. Also the values of symmetry energy at saturation points are listed in Table 1. We observe that the symmetry energy first increases with increasing the Fermi momentum k F until it reaches a maximum value then it decreases with increasing k F .
In Table 2 we present the Fermi momentum at which the symmetry energy takes maximum value k Fmax and it reaches zero k FC (critical Fermi momentum) for various potentials. At high k F the symmetry energy can take negative values, this occurred because at high k F the EoS for symmetric nuclear matter increases more rapidly and in some potentials increase more than the EoS for pure neutron matter. This means that pure neutron matter system becomes more stable than symmetric matter, a phenomenon referred to as isospin separation instability (Li, 2002). Figure 6 shows the energy per nucleon as a function of the density ρ in asymmetric nuclear matter for various values of the asymmetry parameter a. In order to establish the importance of the hole-hole term in the calculated binding energy we have compared BHF calculations (which ignore the hole-hole term) with SCGF, which includes the hole-hole term. As expected, the hh term gives a repulsive contribution to the EoS of asymmetric nuclear matter. This contribution becomes stronger by increasing the density and makes the EoS at high density much stiffer. As the density increases the phase space for the hole-hole propagator is no longer negligible, resulting in an enhanced repulsive effect on the total energy. The additional repulsion from the hh improves greatly the predicted saturation density of cold symmetric nuclear matter. As the neutron density increases (the total density remaining constant), the EoS becomes more and more repulsive. From the figure one notices that, the saturation densities of asymmetric nuclear matter depend on the asymmetric parameter α and the saturation points shift to lower densities. In addition the instability of nuclear matter decreases with increasing asymmetry parameter α, (or decreasing proton fraction).

The Binding Energy
The EoS in the case of asymmetric nuclear matter was studied in more detail in (Gad and Hassaneen, 2007).

The Symmetry Energy and its Relation with the Chemical Potential
Within the parabolic approximation (Equation 16) in (Hassaneen and Gad, 2008) one can obtain the neutron and proton chemical potentials in asymmetric nuclear matter in the following way (Vidana et al., 2000; Equation (30)     where, the minus sign is for neutrons and the plus sign for protons and in particular Equation (31): The nucleon chemical potential difference can be calculated once we have the coefficient of symmetry energy from Equation (31). In Table 3 the shift between neutron and proton chemical potentials µ n -µ p as function of the density for BHF and SCGF approaches using CD-Bonn potential at asymmetry parameter α = 0.8. Reveals that there is a negligible difference between the BHF and the SCGF approximations. This means that the hh ladder brought about negligible contributions to the chemical potential difference specially at high density.

How to Reproduce the Empirical Saturation Point
All results of calculations, which refer to realistic NN interactions, have been obtained using the CD-Bonn (Machleidt et al., 1996) interaction. This includes all BHF and SCGF calculations. Also the evaluation of V lowk has been based on the proton-neutron part of CD-Bonn. The Skyrme Hartree-Fock calculations have been done using the parameterization SLy4 and for the relativistic mean-field calculation the parameterization for DDRMF in (Gögelein et al., 2008) has been used.
First let us turn to the binding energy of symmetric nuclear matter, which are displayed in Fig. 7. Compared to other realistic NN interactions the CD-Bonn potential, which we have chosen here is a rather soft NN interaction with a weak tensor force. This is indicated by the results for the saturation point of symmetric nuclear matter as obtained in the BHF approximation (the minimum of the dashed black line in Fig. 7 and data in Table 4). The saturation density is larger than twice the empirical value and the calculated energy is well below, which means that the CD-Bonn result is located in the large binding energy high density part of the Coester band (Müther and Polls, 2000).
In order to reproduce the empirical saturation point of symmetric nuclear we have added an isoscalar interaction term as defined in Equation (21) choosing a value for δ = 0.5 and fitting the parameters t 0 and t 3 . The results for these fitting parameters are listed in Table 5 and the corresponding energy versus density curves are displayed in Fig. 7.

The Nuclear Compressibility Modulus or the Incompressibility
The results for the calculated saturation points in Table 4 are supplemented by the corresponding values for the nuclear compressibility modulus Equation (32) This nuclear compressibility, which is calculated at the saturation density ρ 0 , together with the increase of energy at large density displayed in Fig. 7 characterize the stiffness of the EoS of symmetric nuclear matter.
Comparing the different approaches we find that the relativistic features included in the DDRMF approach lead to the stiffer EoS around the saturation density as well as at higher densities. The SCGF and the V lowk calculations yield rather similar results after the contact terms are included, which are a little bit softer than the DDRMF results and characterized by a compression modulus of 270 MeV and 258 MeV for SCGF and V lowk , respectively. At higher densities the results are also very close to those obtained for the Skyrme Hartree-Fock using SLy4. Note, however, that SLy4 yields a rather low value for K as compared to the SCGF and V lowk calculations. The softest EoS for symmetric matter among those approaches which fit the empirical saturation point is provided by the BHF approximation. Table 4. Properties of symmetric nuclear matter are compared for Skyrme SLy4, DDRMF, BHF, SCGF and V lowk . The results, which are listed in the columns labeled with +ct are obtained employing the additional contact interaction of Equation (21) with parameters as listed in Table 5. The quantities listed include the saturation density ρ 0 , the binding energy at saturation E=A, the compressibility modulus K and the symmetry energy at saturation density a S (ρ 0 )

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Evaluated for each approach at the corresponding saturation density ρ 0 . The two phenomenological approaches SLy4 and DDRMF yield results which are in the range of the experimental value of 32±1 MeV. Also the BHF and SCGF approach lead to results which are rather close to the empirical value, if the contact term has been added. The BHF and SCGF calculations without the contact term lead to nonrealistic values for a S (ρ 0 ) since these values are calculated at the corresponding saturation densities, which are larger than the empirical saturation density.
The symmetry energy calculated in the SCGF approach is slightly smaller than the one obtained from the BHF approximation. This is valid for all densities under consideration (Fig. 8). This difference can easily be explained: As we already mentioned above, the contribution of the hole-hole terms is repulsive, which leads to larger energies for SCGF as compared to BHF for all densities in symmetric nuclear matter (Fig. 7) as well as in pure neutron matter (Fig. 9). Since, however, the contribution of ladder diagrams is larger in the proton-neutron interaction (due to the strong tensor terms in the 3 S 1 -3 D 1 partial wave) than in the neutron-neutron interaction, this repulsive effect is stronger in symmetric nuclear matter than in neutron enriched matter. Therefore the symmetry energy calculated in SCGF is slightly smaller if the hole-hole terms are included in SCGF (Dieperink et al., 2003). The symmetry energy rises as a function of density for all approaches considered. Note, however, that the two phenomenological approaches Skyrme Hartree-Fock using SLy4 and DDRMF provide rather different predictions at high densities although the symmetry energy at normal density is identical. The relativistic approach predicts symmetry energies for high densities, which are well above all those derived from the microscopic calculations, while the Skyrme interaction yields a symmetry energy which is even below the V lowk estimate at densities above four times saturation density.

β-Equilibrium
Rather similar features also observed, when we inspect the properties of nuclear matter in β-equilibrium, neutralizing the charge of the protons by electrons, displayed in Fig. 10. The upper panel of this figure displays the proton abundance Y p = Z/A, which are to some extent related to the symmetry energy: large symmetry energy should correspond to large proton abundances. So the largest proton abundances are predicted within the DDRMF approach. Already at a density around 0.4 fm −3 Y p exceeds the about 10%, which implies that the direct URCA process could be enabled, which should be reflected in a fast cooling of a neutron star.

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The V lowk and SCGF approaches lead to similar proton abundances at large densities. This demonstrates that the evaluation of the proton abundance in β-equilibrium cannot directly be deduced from the symmetry energy, since the former observable is derived from proton and neutron energies at large asymmetries (Z<<N), whereas the symmetry energy is calculated from the second derivative at N = Z (Equation (28). The BHF approach shows slightly lower values for Y p at high density, but the results are still in the same range as SCGF and V lowk .
At low densities the Skyrme HF approach yields large proton fractions as compared to the results of the other calculations. Large proton fractions at low densities tend to enhance density inhomogeneities and thus favor the existence of a large variety of pasta structures. Therefore the Skyrme HF (Sly4) and the DDRMF approach, which have been explored in detail in (Gögelein et al., 2008;Gögelein and Müther, 2007), should favor the formation of pasta structures as compared to the microscopic approaches. Comparing the energies of matter in β-equilibrium derived from the various approaches as a function of density (Fig. 10, lower panel) we find the same trends as in the case of pure neutron matter displayed in Fig. 9.
The equation of state of nuclear matter in βequilibrium is the main input to predict mass and radii of neutron stars. A stiffer equation of state supports a larger maximum mass and a lower central density. In addition a thicker crust is found for the stiffer equation of state (Engvik et al., 1996).

The Isovector Effective Mass
Another important information for the evaluation of dynamical features of matter in neutron stars is the density of states, which can be characterized by an effective mass. The term effective mass is used in various connections in many-body physics. This includes the effective masses, which express the non-locality of the self-energy in space and time, which corresponds to a momentum and energy dependence. Such effective masses for protons and neutrons determined for nuclear matter in β-equilibrium are displayed in Fig. 11 as a function of density considering non-relativistic approximation schemes.
It is a general feature of all approaches considered that the effective masses for protons as well as neutrons decrease with increasing density. However, there is a striking difference between the phenomenological Skyrme approximation and the BHF and V lowk approach, which are based on realistic NN interactions: The effective mass for protons is smaller than the corresponding one for neutrons in neutron rich matter for the calculations using realistic interactions, while it is opposite applying the Skyrme parameterization. In fact, if we define the effective masses for protons m * It turns out most of the Skyrme parameterizations yield an effective isovector mass * V m , which is even larger than the bare nucleon mass M (Stone and Reinhard, 2007) which implies that it is larger than the effective isoscalar mass * S m . This means that the effective mass for neutrons is smaller than the corresponding one for the protons in neutron rich matter (α>0). These Skyrme parameterizations leading to a large effective isovector mass are usually favored as they correspond within the mean-field approach to an enhancement factor k of the Thomas-Reiche-Kuhn sum-rule (Ring and Schuck, 2004;Bender et al., 2003).
Non-relativistic descriptions of nuclear matter, which are based on realistic interactions yield an effective isovector mass * V m which is smaller than the corresponding effective isoscalar mass, which leads to a larger effective mass for neutrons than for protons in neutron-rich matter (Fig. 11). In order to analyze this finding we inspect the dependence of the nucleon selfenergy in the BHF approximation BHF i ∑ , defined in Equation (7), as a function of energy ω and momentum k of the nucleon considered. Following the discussion of Mahaux and Sartor (1991) one can define the effective k-mass Equation (35): And the effective E-mass Equation (36):  The effective mass can then be calculated from the effective k-mass and the effective E-mass by Equation (37) Results for the effective k-mass and E-mass as obtained from BHF calculations for asymmetric nuclear matter at a density ρ = 0.17 fm −3 and a proton abundance Y p of 25% (α = 0.5) are displayed in Fig. 12. We notice that the effective k-mass for the protons is significantly below the corresponding value for the neutrons at all momenta. Since the k-masses tend to increase as a function of the nucleon momentum k, the difference in the Fermi momenta for protons and neutrons enhance the difference The effective k-mass describes the non-locality of the BHF self-energy. This non-locality and thereby also these features of the effective k-mass are rather independent on the realistic interaction used. Furthermore it turns out that the values for the k-mass are essentially identical if one derives them from the nucleon BHF self-energy using the G-matrix or from the bare interaction V or from V lowk (Frick et al., 2002). This non-locality of the self-energy is dominated by Fockexchange contribution originating from ρ-exchange. In neutron-rich matter this contribution leads to a stronger depletion for the proton mass than for the neutron mass Zuo et al., 2005).
Anyway, the enhancement of the effective mass m*, which is due to the effective E-mass in Equation (32) is not strong enough to compensate the effects of the kmass. Therefore the final effective mass is below the bare mass M and the effective mass for neutrons remains larger than the corresponding one for protons.

The Symmetry Potential Usym
Regarding U n/p as functions of the asymmetry parameter a, one can easily verify that the following approximate relation applies Equation (38): with the ± referring to neutron/proton, respectively. The difference between the neutron and proton potentials then gives an accurate estimate for the strength of the isovector or symmetry potential in asymmetric nuclear matter, i.e., Equation ( figure) and T = 12 MeV (lower one) for symmetric nuclear matter as a function of density using different potentials for continuous choice compared with Argonne V 14 plus microscopic 3BF by Baldo and Ferreira (1999) which is of particular interest and importance for nuclear reactions induced by neutron-rich nuclei. The isovector part of the nucleon potential as a function of nucleon kinetic energy is illustrated in Fig. 13 at asymmetry parameter a = 0.2 (upper panel) and at a = 0.4 (lower panel). The strength of the isovector nucleon optical potential, i.e., the symmetry or Lane potential (Lane, 1962), can be extracted from Equation (34) Figure 13 shows the theoretical symmetry potentials that have been calculated in both BHF and SCGF approaches in comparison with the Lane potential constrained by the experimental data. The vertical bars are used to indicate the uncertainties of the coefficients a and b. It is seen that the strength of symmetry potential decreases with increasing energy .This trend is in agreement with that extracted from the experimental data. At the saturation density, the nuclear symmetry potential is found to change from positive to negative values at a nucleon kinetic energy of about (200 MeV). This is a very interesting result as it implies that the proton (neutron) feels an attractive (repulsive) symmetry potential at lower energies but a repulsive (attractive)

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PI symmetry potential at higher energies in asymmetric nuclear matter. It has been shown that (Zuo et al., 2005) the U sym is almost independent of the isospin asymmetry a within the BHF framework, implying a linear dependence of neutron and proton single-particle potentials on α and providing a microscopic support for the empirical assumption of the Lane potential (Lane, 1962). Also the present results indicate that the U sym is almost independent of the isospin asymmetry a within the BHF and SCGF approaches.

Free Energy of the Symmetric Nuclear Matter at Finite Temperatures
Many attempts were made to use the BHF calculations at finite temperature (Baldo and Ferreira, 1999;Bombaci et al., 2006;Frick and Müther, 2003;Rios et al., 2005). In Fig. 14, the internal energy F of nuclear matter in MeV is plotted against the density ρ in fm -3 and the values obtained with the low temperature expansion (26). The results are shown in Fig. 14, for symmetric nuclear matter using different potentials. For both T = 8 (upper graph) and T = 12 MeV (lower one), for continuous choice. Figure 14 gives the results obtained using the CD-Bonn potential (solid line), the Nijm1 potential (dashed line) and the Reid 93 potential (dashed-dot line) in comparison with a more elaborate calculation using Argonne V 14 plus microscopic 3BF (Baldo and Ferreira (1999)) (dashed double dotted line). From the plotted figures it is observed that the internal energy first decreases with increasing the density until it reaches a minimum then it increases with increasing the density. Our results are comparable to those obtained in (Baldo and Ferreira, 1999).

CONCLUSION
We have investigated the effect of different modern nucleon-nucleon potentials on the EoS, i.e., the nuclear matter binding energy per nucleon, within BHF approach. It is found that our calculations lead to results, which lie along a line (Coester line) shifted with respect to the phenomenological saturation point ( ). We have reviewed the current status of the Coester line, i.e., the saturation points of nuclear matter obtained within BHF approach using the conventional and continuous choice for the auxiliary potential and employing the modern nucleon-nucleon potentials. It is found that our results confirm the concept of a "line", density and energy of the various saturation points being strongly linearly correlated.
We have presented a microscopic calculation of the equation of state of nuclear matte when protons and neutrons have different Fermi momenta. The techniques to evaluate the single-particle green's function in a Self-Consistent G-matrix approach (SCGF). The continuous choice has been adopted for the auxiliary potential. The single-particle energy is calculated self-consistently using BHF and SCGF approximations. The contribution of the hh terms leads to a repulsive contribution to the single-particle energy which decreases with momentum. The dependence of the EoS on the neutron excess parameter is clearly linear as a function of a 2 . The inclusion of the hole-hole ladders and the self-consistent treatment of the Green's function in the SCGF approach leads to a small reduction of the binding energy per nucleon as compared to the BHF approximation.
Various approaches to the nuclear many-body problem have been investigated to explore their predictions for nuclear matter at high density and large proton-neutron asymmetries. Two of these approaches, the Skyrme Hartree-Fock and the Density Dependent Relativistic Mean Field approach are predominantly of phenomenological origin. Their parameters have been adjusted to reproduce data of finite nuclei. However, the parameters have been selected in such a way that also bulk properties of asymmetric nuclear matter derived from microscopic calculations are reproduced. The other three approaches are based on realistic NN interactions, which fit the NN scattering phase shifts. In these approximation schemes (Brueckner Hartree Fock BHF, Self-consistent Greens Function SCGF and Hartree Fock using a renormalized interaction V lowk ) a isoscalar contact interaction has been added to reproduce the empirical saturation point of symmetric nuclear matter.
These various approximation schemes lead to rather similar predictions for the energy per nucleon of symmetric and asymmetric nuclear matter at high densities. In detail one finds that the relativistic DDRMF leads to a rather stiff Equation of State (EoS) for symmetric matter while the BHF approach leads to a relatively soft EoS, a feature which is compensated within the microscopic framework by the repulsive features of the hole-hole ladders included in SCGF. These features are also reflected in the study of nuclear matter in the βequilibrium and lead to moderate differences in the predictions for proton abundances and EoS. More significant differences are observed when we inspect details like the effective masses, in particular the Science Publications PI isovector effective mass. In neutron-rich matter the microscopic approaches predict a positive difference between neutron and proton effective masses. This feature can be related to the non-locality of the selfenergy induced by one-pion exchange term and is expressed in terms of an effective k-mass.
Also the symmetry potential has been calculated as a function of the nucleon kinetic energy. We observe that the strength of the predicted symmetry potential decreases with energy, a behavior which is consistent with the empirical information. It is interesting to note that at normal density (ρ = 0.16 fm −3 ), the nuclear symmetry potential changes from positive to negative values at nucleon kinetic energy around 200 MeV. More details can be read in (Mansour et al., 2010).

ACKNOWLEDGMENT
The researchers would like to thank Prof. H. Müther.