A Self-energy components

# Properties of dense, asymmetric nuclear matter in Dirac-Brueckner-Hartree-Fock approach

## Abstract

Within the Dirac-Brueckner-Hartree-Fock approach, using the Bonn potentials, we investigate the properties of dense, asymmetric nuclear matter and apply it to neutron stars. In the actual calculations of the nucleon self-energies and the energy density of matter, we study in detail the validity of an angle-averaged approximation and an averaging of the total momentum squared of interacting two-nucleons in nuclear matter. For practical use, we provide convenient parametrizations for the equation of state for symmetric nuclear matter and pure neutron matter. We also parametrize the nucleon self-energies in terms of polynomials of nucleon momenta. Those parametrizations can accurately reproduce the numerical results up to high densities.

Dirac-Brueckner-Hartree-Fock approach, asymmetric nuclear matter, equation of state, neutron stars
###### pacs:
21.65.Cd, 26.60.Kp, 24.10.Cn, 21.30.Fe

Also at ]J-PARC Branch, KEK Theory Center, Institute of Particle and Nuclear Studies, KEK, Tokai 319-1106, Japan

## I Introduction

Neutron stars are the most dense and exotic states of nuclear matter in the universe, and it is generally believed that the central density in massive neutron stars reaches several times higher than the normal nuclear density, . Consequently, not only nucleons and leptons but also hyperons may exist stably in the core of neutron star. Because of this extreme situation, observations of neutron stars can provide very important information which cannot be obtained from terrestrial experiments, and thus have recently attracted much attention.

However, the detail of the properties of the core is still in the middle of an argument, although there have been extensive efforts to study it experimentally and theoretically. Because the appearance of hyperons in dense nuclear matter inevitably softens the equation of state (EoS), it is believed that the maximum neutron-star mass becomes seriously diminished if hyperons are created in the core of neutron star. As a result, the majority of theoretical approaches including hyperons, in which Quantum hadrodynamics (QHD) (1) in Hartree approximation (or mean field theory (MFT)) is mostly used, is ruled out by the reliable determination of the mass of pulsar J1614-2230, namely (: the solar mass) (2). (Recently, a new massive pulsar, J0348+0432, has been reported, and the mass is estimated to be (3).)

However, before concluding that the EoS including hyperons cannot explain the heavy neutron stars, it is very important to study the effect of in-medium two-nucleon correlations, which depends on the nuclear density, , on the EoS for the core matter. In this paper, we calculate the properties of dense, asymmetric nuclear matter using the Dirac-Brueckner-Hartree-Fock (DBHF) approach (4); (5); (6); (7); (8); (9); (10); (11), which allows us to handle two vital ingredients: short-range correlations in nucleon-nucleon (NN) force, which are not included in MFT, and relativistic many-body effects.

In MFT, in spite of the considerable uncertainty of nuclear matter properties, the meson-baryon coupling constants are usually adjusted so as to reproduce such data on nuclear matter around . Then, the same coupling constants (without density dependence) are mostly used even in the calculation for neutron stars1. Therefore, such extrapolation to extremely isospin-asymmetric and dense matter like neutron stars may be considered with skepticism.

In contrast, the DBHF calculation is based on the realistic NN interactions, which have been determined using a large amount of NN scattering data, and it can mostly reproduce the nuclear matter properties around without any readjustment of the coupling constants2. The reason for the great success of this method is the density dependence of the in-medium NN scattering amplitude mainly caused by the Pauli exclusion principle, the short-range NN correlations and many-body forces. Thus, it must be important even in the calculation for neutron stars.

However, the DBHF approach is quite complicated and demands enormous time for the calculation. As a result, it is not easy to perform the DBHF calculation for neutron stars even without hyperons, much less the inclusion of hyperons is quite difficult. Thus, it is very vital to reduce the calculation time and costs in order to actually perform the full DBHF calculation including hyperons in the future.

For such purposes, in this work, we study a dimension-reduction approximation in multi-dimensional integrals. In the DBHF approach, it is necessary to work out the coupled, two-dimensional integral equations to obtain the nucleon self-energies. Furthermore, to calculate the energy density of matter, we have to solve the three-dimensional integrals. Such calculations actually require enormous time. Then, to reduce the dimension of integrals and carried out the calculation with less computation time, we exploit an angle-averaged approximation and an averaging of the total momentum squared of interacting two-nucleons in nuclear matter. In particular, we find that the angle-averaged approximation, which has for the first time been used in the DBHF calculation by Horowitz and Serot (1); (4) to study the nuclear matter properties around , is very useful and accurate even in the calculation for dense nuclear matter. We then calculate the mass-radius relation for neutron stars solving the Tolman-Oppenheimer-Volkoff (TOV) equation (14), and examine the validity of those approximations in the calculation for neutron stars.

For practical use, we also provide convenient parametrizations for the EoSs for symmetric nuclear matter and pure neutron matter. In addition, we parametrize the nucleon self-energies in terms of polynomials of nucleon momenta. Those parametrizations can accurately reproduce the numerical results up to high densities ( fm).

The paper is organized as follows. In Sec. II, the DBHF approach is reviewed briefly. In Secs. III.1 , III.2 and III.3, we respectively present the numerical results for the properties of symmetric nuclear matter, the validity of the dimension-reduction approximation and the parametrizations for the nucleon self-energies and the EoSs for nuclear matter. Finally, we give a summary and conclusions in Sec. IV. Throughout this work, we shall use the notation conventions used in Ref. (4).

## Ii Dirac-Brueckner-Hartree-Fock calculation

In the DBHF approximation, the nucleon in asymmetric nuclear matter is described by a set of three, simultaneous integral equations: the Bethe-Salpeter equations, single-particle proper self-energies and Dyson’s equations. The two-nucleon correlations in matter are then expressed by the effective interactions, , which are given by the solutions to the coupled, ladder-approximated Bethe-Salpeter equations:

 Γdir,exii = Vdir,exii+∫Vdir,exiiQavii~giiΓdir,exii , (1) Γdirij = Vdirij+∫VdirijQavij~gijΓdirij+∫VexijQavji~gjiΓexij , (2) Γexij = Vexij+∫VexijQavij~gijΓdirij+∫VdirijQavji~gjiΓexij , (3)

where or denotes neutron () or proton (), and the superscript, , stands for the direct (exchange) term in the two-nucleon scattering. The ladder-approximated Bethe-Salpeter equations sum to all orders the one-boson-exchange (OBE) interactions, , between two nucleons. Here, is the angle-averaged Pauli exclusion operator, and denotes an approximated two-nucleon propagator (4). The use of these quantities allows us to reduce the four-dimensional integral equations, Eqs. (1) - (3), to two-dimensional ones, which makes the further numerical calculation in the center-of-mass frame of the interacting two nucleons feasible. In the present calculation, as , we use the Thompson propagator, (15).

The self-energy, , is connected to the effective interaction in a nuclear medium by summing up all orders of direct and exchange diagrams. It is given by

 Σi=−i∑j=p,n∫[tr(GjΓdirij)−GjΓexij] , (4)

where is the Green’s function of interacting nucleon. In addition to Eqs. (1)-(4), to impose self-consistency, the Dyson’s equation must be satisfied:

 Gi=G0i+G0iΣiGi , (5)

where is the Green’s function in free space. If the higher-order diagrams in Eqs. (1)-(3) are ignored, the above procedure coincides with relativistic Hartree-Fock approximation. In addition, if we ignore the exchange diagram in Eq. (4), the relativistic Hartree (or MFT) result is reproduced.

The self-energy in a uniform matter can generally be written as

 Σi(k)=ΣSi(k)−γ0Σ0i(k)+γ⋅kΣVi(k), (6)

with () being the three- (four-) momentum. Here, is the scalar (the zero-th component of vector) [the space component of vector] part of the nucleon self-energy. The actual calculation for these self-energy components is explained in Appendix A.

Using the self-energies, the effective nucleon mass, , and the single-particle energy, , in matter are obtained as

 M∗i = MN+ΣSi(kFi,E∗i(kFi))1+ΣVi(kFi,E∗i(kFi)) , (7) Ei(k) = E∗i(k)−Σ0i(kFi,E∗i(kFi))+E∗i(k)ΣVi(kFi,E∗i(kFi)) , (8)

with being the free nucleon mass, and being the Fermi momentum of nucleon . The Dirac equation in matter then reads

 [α⋅k+βM∗i]ui(k,λ)=E∗i(k)ui(k,λ) , (9)

with the solution with helicity, ,

 ui(k,λ)=√E∗i(k)+M∗i⎛⎝[]c12λk––E∗i(k)+M∗i⎞⎠χλ , (10)

where and is the Pauli spinor. This solution is normalized as .

The energy density of nuclear matter, , is composed of the kinetic and potential energies, which are given in terms of as

 E=∑i=p,n(⟨^Ti⟩+∑j=p,n⟨^Vij⟩) , (11)

with

 ⟨^Ti⟩ = kFi8π2(k2Fi+M∗2i)1/2[4MiM∗i−3M∗2i+2k2Fi] (12) +M∗3i8π2[3M∗i−4Mi]log(kFi+(k2Fi+M∗2i)1/2M∗i) , ⟨^Vij⟩ = ∫d3p(2π)3∫d3P(2π)3θ(kFi−∣∣12P+p∣∣)2E∗i(12P+p)θ(kFj−∣∣12P−p∣∣)2E∗j(12P−p)~Γij , (13)

where and are, respectively, the total and relative momenta for the interacting two nucleons in the matter-rest frame. Using the spinor, Eq. (10), in that frame, the matrix element, , is calculated by

 ~Γij = Missing or unrecognized delimiter for \right (14) Missing or unrecognized delimiter for \right

The calculation of the potential part, Eq. (13), is explained in Appendix B.

## Iii Numerical results

We present our results of the DBHF calculation, in which we use the Bonn potentials for the NN interaction (6) and the subtracted T-matrix representation explained in Appendix A (see also Ref. (8)). There are three kinds of Bonn potentials, namely Bonn A, B and C, where the NN potential is generated by the exchanges of , , , , and mesons, and is parametrized so as to reproduce the deuteron properties and the phase shifts of NN scattering (6); (16). The difference among the three potentials is primarily caused by the strength of the tensor force.

In this paper, our calculation mainly follows the method given in Ref. (4). However, we use the subtracted T-matrix representation (8) in the self-energy calculation. As we will see below, the present results are, however, slightly different from those in Ref. (8), even though we employ the same subtracted T-matrix representation as in Ref. (8). The reason for it is that, in the calculation of the energy density at the matter-rest frame, we directly use the matrix elements of given in Eq. (14), which remain unchanged under Lorentz transformation, while, in Ref. (8), the energy density is calculated by Eq. (29) in Ref. (7), in which, instead of , the self-energies at the rest frame are used. However, in spite of this difference, the result in Ref. (8) is very close to the present one up to high densities.

Because various results for nuclear matter given by the DBHF calculation have already been reported elsewhere (4); (5); (6); (7); (8); (9); (10); (11), we here focus on two topics: (1) the validity of the angle-averaged approximation and the averaging of the total momentum squared of the interacting two nucleons in matter, (2) parametrizations for the nucleon self-energies and the EoSs for symmetric nuclear matter and pure neutron matter.

### iii.1 Properties of nuclear matter in the DBHF approach

Before we present the main result, we summarize our results for the properties of nuclear matter. In Fig. 1, we show the binding energies per particle for symmetric nuclear matter and pure neutron matter in the vicinity of saturation density, . In the figure, the rectangular area shows the region of saturation point for symmetric nuclear matter suggested by various semi-empirical data (17), that is MeV, and the Fermi momentum, fm.

We can see that the saturation points calculated by Bonn A and B are in the rectangular region (see also Table 1, in which we list the several properties of symmetric nuclear matter at the saturation points). On the other hand, the result of Bonn C is located outside the region. It may implies that the strength of the tensor force in the interaction strongly relates to the position of the saturation on the Coester band. Therefore, it might be interesting to take the averaged values of parameters for the Bonn A and B potentials (which we call Bonn AB) and see how such parameters give the saturation properties. The result of Bonn AB is also shown in Fig. 1 and Table 1. From the figure, as expected, we can see that the resulting saturation point lies in between those of Bonn A and B.

For the case of pure neutron matter, the binding energies for Bonn A, B, C and AB are very close one another, because the tensor force mainly influences the coupled states in the two-nucleon system with total isospin , and thus it gives less impact on pure neutron matter (18).

We comment on the properties of symmetric nuclear matter. In MFT, it is indispensable to include nonlinear -meson terms phenomenologically to obtain the correct value of the nuclear incompressibility, MeV (19). In contrast, it is not necessary to consider such nonlinear terms in the DBHF approach. It is remarkable that, in the Bonn A, the incompressibility, , is estimated to be MeV. However, the symmetry energy, , and the slope parameter, , in Bonn A are slightly larger than the values suggested in Ref. (20). This may be caused by the fact that the saturation point in Bonn A is located at the relatively deeper binding energy and higher density in the allowed, rectangular region. We note that the present DBHF calculation can provide the similar results of the density dependences of symmetry energy and the pressure for symmetric matter to those calculated in Ref. (9); (10).

Hereafter, we shall use the Bonn A potential as the optimum interaction.

### iii.2 Dimension-reduction approximation for multi-dimensional integrations

To perform a realistic calculation of the EoS for neutron stars, it is necessary to take into account the N-hyperon (Y) and YY interactions as well as the NN interaction, in which we have to consider a lot of two-baryon channels. Because such calculations should be carried out in a wide range of nuclear densities, for example, , we need an enormous amount of calculation time. As an attempt to reduce calculation time, we study a dimension-reduction approximation for multi-dimensional integrations in the calculations of self-energies and energy density.

In the self-energy calculation, the components, and , are calculated by two-dimensional integral equations (see Eqs. (23) - (28) in Appendix A). We here try to reduce those to one-dimensional ones by exploiting the angle-averaged approximation (see Appendix A and Ref. (4)). We respectively call the self-energies calculated by the two-dimensional integral equations and those by the one-dimensional ones and .

In Fig. 2, we show the results of and in symmetric nuclear matter as a function of the total baryon density, .

As seen in Fig. 2, the curves of agree very well with those of , i.e. the full calculations, over a wide range of density, which implies that the angle-averaged approximation in the self-energy works very well. As a consequence, we can replace by not only at low densities but also at high densities.

The potential energy, , in the energy density is calculated by the three-dimensional integral (Eq. (42) in Appendix B), and thus, it is necessary to somehow approximate it. By assuming the angle-averaged approximation, we can again reduce the three-dimensional integral to two-dimensional one. We call the result with this assumption , while we call the result of the full calculation . In addition, if we adopt the averaging of the total momentum squared of the interacting two nucleons in matter, the two-dimensional integral is further reduced to one-dimensional one (see Appendix B). We call this result .

In Fig. 3, we compare the full result, , with the approximated ones, and . The three solid (or dashed) curves are in good agreement below . However, increasing the total baryon density, increases the discrepancy between and , which implies that the full calculation cannot be approximated by at high densities. In contrast, the difference between and is still rather small even at high densities.

Next, using , we calculate the neutron-star mass as a function of the radius, which is given in Fig. 4. We also list the properties of neutron stars in Table 2. The present calculation is restricted to the neutron-star matter composed of protons, neutrons, electrons and muons. Under the conditions of charge neutrality and -equilibrium in weak interaction, we solve the TOV equation (14) to obtain the mass-radius relation. So far, in the DBHF calculation, the EoS for neutron-star matter is calculated by using the parabolic interpolation between the EoSs for symmetric nuclear matter and pure neutron matter (see, for example, Ref. (10); (11)). However, in the present work, we calculate the EoS for asymmetric nuclear matter without such interpolations.

As expected from the result shown in Fig. 3, the EoS by gives the heaviest mass, , and the large difference between the maximum masses by and is seen in Fig. 4. However, the mass by is very close to that by .

Thus, we can conclude that the combination of approximations, and , to the calculations of self-energies and energy density is the most suitable one to save calculation time. Furthermore, we may be able to expected that the difference between and becomes smaller in the neutron star containing hyperons as well as nucleons, because the creation of hyperons reduces the fraction of nucleon density in matter, and thus the high density part in Fig. 3 may not contribute much to the EoS in such cases.

### iii.3 Parametrizations

For convenient use of the DBHF result, we provide useful parametrizations for the self-energy components and the EoS for nuclear matter.

Each component of the nucleon self-energy, which depends on the momentum, , and the Fermi momentum, ( or ), can be parametrized by the following, power-series expansion:

 ΣSn(kFn,kFp,k) (15) = −1033+2284kFn−1767k2Fn+425.2k3Fn−29.29k4Fn+384.9kFp−386.3kFnkFp +148.3k2FnkFp−25.01k3FnkFp−201.2k2Fp+94.37kFnk2Fp−5.789k2Fnk2Fp−32.46k3Fp −2.635kFnk3Fp+12.54k4Fp+172.1k−267.1kFnk+102.0k2Fnk−10.51k3Fnk−71.29kFpk +10.60kFnkFpk+16.66k2FnkFpk+36.53k2Fpk−16.82kFnk2Fpk−3.828k3Fpk−52.33k2 +136.6kFnk2−31.39k2Fnk2+25.97kFpk2−16.83kFnkFpk2+7.546k2Fpk2−45.74k3 +2.287kFnk3−0.8569kFpk3+6.430k4 ,
 ΣSp(kFn,kFp,k) (16) = −893.2+1869kFn−1423k2Fn+380.5k3Fn−32.92k4Fn+545.7kFp−687.3kFnkFp +239.8k2FnkFp−28.93k3FnkFp−107.3k2Fp+224.8kFnk2Fp−27.68k2Fnk2Fp−231.1k3Fp −21.26kFnk3Fp+60.10k4Fp+54.78k+13.65kFnk+19.75k2Fnk−0.4057k3Fnk−105.2kFpk −56.77kFnkFpk−11.83k2FnkFpk+68.64k2Fpk+30.57kFnk2Fpk−19.26k3Fpk−87.59k2 +24.20kFnk2−7.972k2Fnk2+86.62kFpk2+7.563kFnkFpk2−8.808k2Fpk2+7.976k3 +0.7710kFnk3−25.90kFpk3+7.593k4 ,
 Σ0n(kFn,kFp,k) (17) = 191.6−573.1kFn+515.9k2Fn−245.7k3Fn+17.55k4Fn−88.93kFp+111.9kFnkFp −45.05k2FnkFp−1.718k3FnkFp+113.6k2Fp−58.68kFnk2Fp+21.11k2Fnk2Fp−56.05k3Fp −4.129kFnk3Fp+1.502k4Fp+202.5k−203.2kFnk−0.6211k2Fnk+17.24k3Fnk−45.30kFpk +8.512kFnkFpk+19.11k2FnkFpk+19.44k2Fpk−22.48kFnk2Fpk+3.111k3Fpk−112.8k2 +174.3kFnk2−22.86k2Fnk2+10.78kFpk2−15.74kFnkFpk2+9.332k2Fpk2−28.79k3 −19.35kFnk3+1.244kFpk3+12.31k4 ,
 Σ0p(kFn,kFp,k) (18) = −37.78+84.47kFn+30.83k2Fn−75.99k3Fn+6.714k4Fn−31.29kFp−60.14kFnkFp +38.01k2FnkFp−10.13k3FnkFp+19.28k2Fp+31.65kFnk2Fp+10.98k2Fnk2Fp−79.14k3Fp −27.68kFnk3Fp+6.778k4Fp−8.749k+44.05kFnk−0.004370k2Fnk+0.01541k3Fnk +25.79kFpk−47.72kFnkFpk+1.585k2FnkFpk−36.53k2Fpk+8.365kFnk2Fpk+13.95k3Fpk −56.79k2−15.44kFnk2+1.677k2Fnk2+49.77kFpk2+9.450kFnkFpk2+10.32k2Fpk2 +28.56k3−0.02399kFnk3−37.12kFpk3+9.125k4 ,
 ΣVn(kFn,kFp,k) (19) = 0.1521−0.5998kFn+0.8179k2Fn−0.4307k3Fn+0.06665k4Fn−0.2702kFp+0.2533kFnkFp −0.1394k2FnkFp+0.03638k3FnkFp+0.3053k2Fp+0.0007945kFnk2Fp−0.001880k2Fnk2Fp −0.2312k3Fp−0.01501kFnk3Fp+0.05148k4Fp+0.3278k−0.6618kFnk+0.4069k2Fnk −0.07270k3Fnk−0.05230kFpk+0.03404kFnkFpk−0.05118k2FnkFpk+0.02249k2Fpk +0.05848kFnk2Fpk−0.02161k3Fpk+0.08527k2−0.1199kFnk2+0.03291k2Fnk2 +0.0006560kFpk2+0.02024kFnkFpk2−0.01927k2Fpk2+0.02552k3−0.006904kFnk3 −0.0008859kFpk3−0.002613k4 ,
 ΣVp(kFn,kFp,k) (20) = 0.1887−0.1975kFn+0.1287k2Fn−0.08467k3Fn+0.01424k4Fn−0.6801kFp+0.5139kFnkFp −0.1847k2FnkFp+0.02296k3FnkFp+0.6572k2Fp−0.1481kFnk2Fp+0.02273k2Fnk2Fp−0.3207k3Fp +0.01080kFnk3Fp+0.05429k4Fp+0.1452k−0.08241kFnk+0.07264k2Fnk−0.01388k3Fnk −0.1953kFpk−0.06356kFnkFpk+0.001918k2FnkFpk+0.1436k2Fpk+0.02130kFnk2Fpk −0.03376k3Fpk−0.05190k2+0.01251kFnk2+0.003157k2Fnk2+0.05247kFpk2 −0.006964kFnkFpk2−0.007900k2Fpk2−0.004147k3−0.002807kFnk3+0.002096kFpk3 −0.0006445k4 .

These are fitted so as to reproduce the results of the full () calculation with Bonn A, and valid for the region of , and for , where is the proton fraction, , with being the proton density.

In addition, we also provide parametrizations for the EoSs for symmetric nuclear matter (s.n.m.) and pure neutron matter (n.m.) in terms of polynomials of the nuclear density:

 (EnB−MN)s.n.m. = {−4.570−130.4nB+326.1n2B+144.5n3B for 0

where is in fm. These are again fitted to the results of the full calculation with Bonn A. In Eqs. (21) and (LABEL:eq:binding_energy_nm_fit), the density region is divided into two parts at fm, and, at that density, the value of polynomial function and its derivative are respectively continuous. These parametrizations are shown in Fig. 5, and they work very well up to very high density.

For the calculation of asymmetric nuclear matter, it may practically be convenient to use the parabolic interpolation between Eqs. (21) and (LABEL:eq:binding_energy_nm_fit), because the difference between the results by the interpolation and is not large (see Fig. 6).

## Iv Summary and conclusions

Using the DBHF approximation, we have investigated the properties of isospin-asymmetric nuclear matter not only in the vicinity of saturation density but also for high densities, and have applied the DBHF approach to neutron stars.

We have first confirmed that the present DBHF approach, in which the subtracted T-matrix representation is applied to the Bethe-Salpeter equations with the Bonn potentials, can mostly explain the observed, saturation properties of symmetric nuclear matter. Next, since the DBHF calculation is very complicated and needs enormous calculation time, to handle it as easily as possible, we have examined a dimension-reduction approximation, namely the angle-averaged approximation and the averaging of the total momentum squared of the interacting two nucleons in matter, in the calculations of nucleon self-energies and energy density of matter.

By applying the angle-averaged approximation, the self-energy components can be calculated very accurately by the one-dimensional integral equations up to high densities (). However, in the calculation of energy density, which requires the three-dimensional integral, the validity of the dimension-reduction approximation depends on the total baryon density, that is, by applying both the angle-averaged approximation and the averaging of the total momentum squared of two nucleons, the three-dimensional integral can be well approximated by the one-dimensional one in the vicinity of saturation density, , while, at high densities, the averaging of the total momentum squared does not work well, and thus we must at least handle the two-dimensional integral.

In the present paper, we have provided simple and useful parametrizations for the nucleon self-energies and the EoSs for symmetric nuclear matter and pure neutron matter, which are fitted so as to reproduce the results of the full DBHF calculation and cover the density range of .

Finally, we comment on future works. We have not considered the degrees of freedom of hyperons in the present calculation. It is generally believed that the inclusion of hyperons in neutron stars inevitably softens the EoS and thereby the maximum mass of neutron star is seriously reduced. However, it might be premature to conclude so, because, within relativistic Hartree-Fock approximation, the creation of hyperons in neutron stars is strongly suppressed and thus the EoS is not so soften (13). In any case, it is very vital to perform the full DBHF calculation including hyperons as well as nucleons to address this issue. The dimension-reduction approximation we have proposed in the present paper may help us accomplish such heavy DBHF calculations.

It is also important to consider the - and -meson exchanges between two baryons in matter. In MFT, they do not contribute to the EoS because of the absence of Fock diagrams. When the Fock terms are taken into account, the - and -meson exchanges mix some baryons in matter. The and mesons also mix the and through the Fock diagrams.

At very high density, the quark and gluon degrees of freedom, rather than the hadron degrees of freedom, take place in neutron stars (21). Thus, it is eventually necessary to take into account such degrees of freedom and consider the phase transition between the quark-gluon and hadron phases.

###### Acknowledgements.
This work was supported by JSPS KAKENHI Grant Number 255742. We thank Tomoyuki Maruyama and N. Yasutake for valuable suggestions.

## Appendix A Self-energy components

The effective interactions, , in the ladder-approximated Bethe-Salpeter equations, Eqs. (1)-(3), are most conveniently calculated in the center-of-mass frame of the interacting two nucleons. In contrast, using the , the self-energies, Eq. (4), must be calculated in the matter-rest frame. Therefore, the effective interactions, , have to be transformed between the two frames.

The present calculation of the self-energies follows the works by Faessler’s group (8); (9), where they have proposed the subtracted T-matrix representation which is composed of pseudoscalar (ps) and complete pseudovector (pv) representations. The complete pv representation is then applied to the effective interaction due to the single - and -meson exchanges, while the ps representation is used for the multiple - and -meson exchanges and the other heavy-meson exchanges.

The effective interaction is divided into five Lorentz-covariants, that is, the scalar (), vector (), tensor (), axial-vector () and pseudoscalar () components in the ps representation, while, instead of , the pseudovector () component takes place in the pv representation. Moreover, by setting a different type of pv representation, one can get rid of undesired ps contributions due to the -meson exchange. This new one is designated as the complete pv representation (8).

In the ps representation, the components of on-shell self-energy are given by

 ΣSi(k––,E∗i(k)) (23) = ∑j=p,n∫d3q(2π)3M∗jE∗j(q)θ(kFj−|q|)(2SΓdirij−12∑mξmsmΓexij) , Σ0i(k––,E∗i(k)) = −∑j=p,n∫d3q(2π)3θ(kFj−|q|)(2VΓdirij−12∑mξmvmΓexij) , (24) ΣVi(k––,E∗i(k)) = −∑j=p,n1k––2∫d3q(2π)3q⋅kE∗j(q)θ(kFj−|q|)(2VΓdirij−12∑mξmvmΓexij) , (25)

with and being the exchange coefficients (see Table 3). In the complete pv representation, they are written as

 ΣSi(k––,E∗i(k)) (28) = ∑j=p,n∫d3q(2π)3θ(kFj−|q|)M∗j2E∗j(q)[4(Sgdirij+~Sgexij)−(Sgexij+~Sgdirij)+4(Agexij+Agdirij) −1(M∗i+M∗j)2{M∗2i+M∗2j−2(E∗i(k)E∗j(q)−k⋅q)}(PVgexij+~PVgdirij)] , Σ0i(k––,E∗i(k)) = ∑j=p,n∫d3q(2π)3θ(kFj−|q|)2{(Sgexij+~Sgdirij)−2(Agexij+Agdirij) +1(M∗i+M∗j)2E∗j(q)[2E∗i(k)(M∗2j−E∗j(q)E∗i(k)+q⋅k) −E∗j(q)(M∗2j−M∗2i)](PVgexij+~PVgdirij)} , ΣVi(k––,E∗i(k)) = ∑j=p,n1k––2∫d3q(2π)3θ(kFj−|q|)2E∗j(q){q⋅k[(Sgexij+~Sgdirij)−2(Agexij+Agdirij)] −1(M∗i+M∗j)2[−2k––2(M∗2j−E∗j(q)E∗i(k)+q⋅k) −q⋅k(M∗2i−M∗2j)](PVgexij+~PVgdirij)} ,

with a linear transformation

 ⎡⎢ ⎢ ⎢ ⎢ ⎢ ⎢ ⎢ ⎢ ⎢ ⎢⎣Sgdir,exij~Sgdir,exijAgdir,exijPVgdir,exij~PVgdir,exij⎤⎥ ⎥ ⎥ ⎥ ⎥ ⎥ ⎥ ⎥ ⎥ ⎥⎦=14⎡⎢ ⎢ ⎢ ⎢ ⎢ ⎢⎣4−2−80−20−6−16020200202−84206−160−2⎤⎥ ⎥ ⎥ ⎥ ⎥ ⎥⎦⎡⎢ ⎢ ⎢ ⎢ ⎢ ⎢ ⎢ ⎢ ⎢ ⎢⎣SΓdir,exijVΓdir,exijTΓdir,exijPVΓdir,exijAΓdi