Charged ρ Meson Condensate in Neutron Stars within RMF Models

Knowledge of the equation of state (EoS) of cold and dense baryonic matter is essential for the description of properties of neutron stars (NSs). With an increase of the density, new baryon species can appear in NS matter, as well as various meson condensates. In previous works, we developed relativistic mean-field (RMF) models with hyperons and ∆-isobars, which passed the majority of known experimental constraints, including the existence of a 2 M neutron star. In this contribution, we present results of the inclusion of ρ−-meson condensation into these models. We have shown that, in one class of the models (so-called KVOR-based models, in which the additional stiffening procedure is introduced in the isoscalar sector), the condensation gives only a small contribution to the EoS. In another class of the models (MKVOR-based models with additional stiffening in isovector sector), the condensation can lead to a first-order phase transition and a substantial decrease of the NS mass. Nevertheless, in all resulting models, the condensation does not spoil the description of the experimental constraints.


Introduction
The equation of state (EoS) of strongly interacting hadronic matter is an essential input for describing the properties of neutron stars (NSs).A viable EoS has to fulfill various constraints following from both astrophysical observations and nuclear experimental data [1].The discovery of the most massive pulsar with the mass M = 2.01 ± 0.04 M [2] put a severe constraint, ruling out many soft EsoS.Currently, one of the most challenging tasks for phenomenological models of the EoS is to pass simultaneously the maximum NS mass constraint, requiring the EoS to be stiff, and the so-called flow constraint [3] coming from the analysis of flows in heavy ion collisions, which requires a soft EoS.This is hard to achieve within traditional models.
Relativistic mean-field (RMF) framework is a convenient and successful tool for constructing the nuclear equation of state.With an increase of the density hyperons and ∆ isobars can appear in the NS matter [4].In most of known model, this leads to a decrease of the maximum NS mass to unrealistic values.Another reason of the EoS softening is the possible appearance of the charged ρ-meson condensate in NS matter [5].An RMF EoS can be made more flexible by introducing the dependence on the scalar field of the effective couplings and masses of all hadrons.In [6], we constructed new models within this approach, which fulfill the maximum NS mass constraint and the flow constraint simultaneously together with many other constraints, even with hyperons and ∆ isobars included.In the current contribution, we demonstrate results of the inclusion of the charged ρ-meson condensate into our models.More details on the calculations can be found in [7].

Description of the Model
Our model was initially formulated in [8] and extended in [6,7,9].Without the ρ − meson condensation, the energy density of the model reads: Here, we introduced the dimensionless scalar field f = g σN χ σN (σ)σ/m N .The isospin projection of baryon b is t 3b , and p F,j = (6π 2 n j /(2s j + 1)) 1/3 denotes the Fermi momentum of a fermion j, with s j and n j being the spin and density of a species j, respectively, j = (b, l), l labels leptons.In the infinite hadronic matter without meson condensates, the energy density depends only on the ratios of the meson coupling constants, masses and their corresponding scaling functions, namely Here, the the self-interaction potential U(σ) entering the Lagrangian of the model is hidden into the scaling function η σ ( f ).The coupling constant ratios for various baryons are defined as x Mb = g Mb /g MN , x φH = g φH /g ωN .We refer the reader to [6,9] for explicit expressions for the scaling functions η m ( f ) and values of the parameters for all our models.Below, we use χ Mb = χ MN , χ φH = 1.
The baryon coupling ratios with vector mesons x ωB and x ρB are determined by the quark SU(6) symmetry.The baryon coupling ratios with the scalar field x σB follow from the potentials in the isospin-symmetric matter (ISM) at the saturation density n = n 0 .The ∆ potential U ∆ (n 0 ) ≡ U ∆ is a subject of large uncertainties.Here we assume U ∆ = −50 MeV, following from the most realistic estimate [10].The values of the parameters for all included baryon species are given in [6].

Charged ρ Condensate
The ρ meson field is described by the following Lagrangian [5,8] where the chemical potential µ ch,ρ is introduced for charged mesons and ( n 3 ) a = δ a3 is the unit vector in the isospin space.We treat ρ meson as a gauge boson of a hidden local symmetry and introduce the non-Abelian coupling constant g ρ and its scaling function χ ρ ( f ).Hidden local symmetry requires that g ρ = g ρN , which we use here, and for simplicity we consider χ ρ ( f ) = 1.In the standard ansatz for the ρ-meson mean fields only the ρ (3) 0 component is non-zero.This ansatz was used in obtaining Equation (3).The charged ρ − meson condensation can be introduced by using the new ansatz for the ρ meson field: It can be shown that within this ansatz the minimum of energy is realized if the condition is fulfilled.This is equivalent to the ratio ρ being constant and independent of the spatial index i.Thus we can assume that ρ , where we defined the complex amplitude of the charged ρ meson field ρ c , and a = {a i } is the spatial unit vector.In such terms the thermodynamic potential can be minimized by two distinct solutions for the ρ The electric charge density of The ρ − meson condensate gives the following contribution to the energy density: where θ(−n I − n ρ ) = 1 for n I + n ρ < 0 and zero otherwise.In the presence of the condensate, the charge neutrality condition is modified to be ∑ b Q b n b − n e − n µ + n ch,ρ = 0.In the beta-equilibrium matter (BEM) of a NS the chemical potentials are related through conditions All equations are solved self-consistently with the equation of motion for the scalar field ∂(E + µ ch,ρ n ch,ρ )/∂ f = 0. Once the equilibrium concentrations are obtained, the pressure can be evaluated as P = ∑ j=b,l,{ch,ρ} µ j n j − E.

Numerical Results
In [7], we considered the MKVOR* and KVORcut03 model.We have shown that, in the KVORcut03 model, the ρ − condensate does not appear in the most realistic case with the hyperons and/or ∆s taken into account.Thus, in this contribution, we focus on results for the MKVOR* model.Below, we present the results of the inclusion of the ρ − condensate into the MKVOR* model with the universal mass scaling and check the sensitivity of the results to varying the scaling functions Φ ρ ( f ) and η ρ ( f ).In the following, we denote the MKVOR* model with hyperons and ∆s included as MKVOR*H∆φ, and the inclusion of ρ − condensate is denoted by the ρ suffix.

Inclusion of the Condensate
In this section, we present the results for the MKVOR* model with the universal meson mass scaling Φ m ( f ) = 1 − f , m = {σ, ω, ρ, φ}, in accordance with [11][12][13].In the left panel of Figure 1, we show the particle concentrations and the scalar field f as functions of the total baryon densities.There exists a region of densities where several solutions for the particle fractions and the scalar field exist.This means that the system must prefer the branch of solutions with a lower energy.The density, for which such a transition from one branch of solutions to another happens, in our model, equals n (I) c = 2.81 n 0 .It is shown in Figure 1 by dotted vertical lines in the left and middle panels.The 1st order PT results in a van der Waals-like shape of the pressure, which, neglecting the possible pasta formation, should be replaced by a Maxwell construction, spanning over the densities 2.37 n 0 n 3.37 n 0 .The resulting pressure as a function of the density is shown in the middle panel of Figure 1, where we compare the pressure with and without condensate for the MKVOR*H∆φ model.The condensate appears not only on the new branch of solutions, but also at the old one with the critical density n (II) c 2.74 n 0 , which is marked by a horizontal dash.In the right panel of Figure 1, we show the NS mass as a function of the central density for MKVOR*H∆φ with and without the inclusion of the condensate.We see that the ρ − condensation in this model results in a substantial decrease of the maximum NS mass from 2.21 M to 2.03 M .Nevertheless, even after such a reduction, the NS maximum mass still passes the observational constraint.

Variation of the ρ-Meson Effective Mass
A strong phase transition to the ρ − -condensed state relies on the strong decrease of its effective mass.In this subsection, we study the effect of limiting the decrease of the ρ-meson effective mass using the following mass scaling function: This expression defines a one-parametric family of scaling functions, with a minimum value of the function Φ ρ,min as the parameter.For a given Φ ρ,min , the value of f s is where we introduce a constant offset δΦ ρ = 0.1 allowing for a smooth transition at f = f s .
The resulting pressure as a function of the density is shown in the middle panel of Figure 2. The 1st order PT proves to be present for Φ ρ,min < 0.7.However, the corresponding critical density grows and the pressure loss decreases as we increase Φ ρ,min .For Φ ρ,min = 0.7 no condensate appears in the model.The mass-radius curves for this models are shown in the right panel of Figure 2. The limiting of the decrease of Φ ρ ( f ) leads to an increase of the maximum NS mass.The maximum NS mass Φ ρ,min = 0.3, 0.5, 0.7 are 2.06, 2.16, and 2.21 M , respectively, proven to be larger than 2.03 M in the case of Φ ρ ( f ) = 1 − f .Thus taming the ρ-meson effective mass decrease is an efficient way to control the effect of the ρ − condensate.

Variation of the η ρ ( f )
Another reason for the large ρ − condensate fraction is the particular shape of the η ρ ( f ) function in the MKVOR* model.The sharp decrease in the η ρ ( f ) for f 0.5 is needed to quench the scalar field growth in the isospin-asymmetric matter, implementing the cut-mechanism of stiffening of the EoS [22].However, as we shall see in this section, this choice of η ρ ( f ) corresponds to the maximum ρ − condensate in the NS matter.To show this, we investigate a set of scaling functions η ρ ( f ), smoothly changing their behavior from a sharp decrease at f 0.5 to a monotonous growth for all f .
The family of η ρ ( f ) we use here consists of functions η (i) ρ ( f ), i = 1 . . .17 within three different analytic parameterizations labeled by an integer number.The details on the parameterizations can be found in [7].The choice of η (1) ρ corresponds to the original η ρ ( f ) of the MKVOR* model (tail 2).Dependence of η (i) ρ ( f ), i = 1 . . .17 on the scalar field f is shown in the left panel of Figure 3.We see that with an increase of the model number gradually changes the η (i) ρ behavior from sharply decreasing for f 0.5 to a monotonously growing function, thus switching off the cut-mechanism [22], which limits the growth of the scalar field.
In the right panel of Figure 3, we show the maximum NS mass as a function of the model index, while varying number of degrees of freedom included.Namely, we study the MKVOR*{Hφ, H∆φ, Hφρ, H∆φρ} models with Φ ρ ( f ) = 1 − f .For estimating the effect of limiting the decrease of the ρ-meson effective mass on these curves we consider also the MKVOR*H∆φρ model with Φ ρ given by Equation (7) with Φ ρ,min = 0.5.For the models without ρ − condensate we see, that the choice maximizes the maximum NS mass, thus proving the efficiency of our "cut" mechanism of the EoS stiffening.In addition, one should notice that the difference between Hφ and H∆φ curves is as well minimized by the η (1) ρ .It means that this choice of η ρ plays an important role in resolution of the "∆ puzzle" [23].With an increase of the model number the impact of ∆s on the EoS grows, and for i = 17 the maximum NS mass becomes 2.03 M , marginally satisfying the maximum NS mass constraint.
The inclusion of the ρ − condensate changes this tendency.The Hφρ curve monotonously increases with an increase of the model index and the choice η ρ = η (1) ρ minimized the maximum mass and maximizes the ρ − condensate phase transition strength.A peculiar situation occurs if both ∆s and ρ − are included into the model.As one sees from the H∆φρ curve in the right panel of Figure 3, the maximum NS mass is close to 2.03 , M and almost independent on the model index.This happens because for low i → 1 the softening comes from both the ρ − condensate together with ∆s, and for large i → 17 the ρ − condensate disappears and the softening effect of ∆s is increased, as was mentioned above.However, this independence of a maximum NS mass on the model number is accidental and holds only for Φ ρ = 1 − f .If we limit the decrease of the ρ-meson effective mass (see H∆φρ, Φ ρ,min = 0.5 curve in the right panel of Figure 3), such a degeneracy is removed.ρ for i = 1 . . .17 as functions of the scalar field f .Right panel: Maximum NS mass as a function of the model number for MKVOR*{Hφ, H∆φ, Hφρ, H∆φρ} models with Φ ρ ( f ) = 1 − f and for MKVOR*H∆φρ with Φ ρ given by Equation (7) with Φ ρ,min = 0.5.

Conclusions
We studied a possibility of charged ρ-meson condensation in a realistic relativistic mean-field model MKVOR* with scaled hadron masses and couplings.The condensation proves to happen by a first-order phase transition and leads to a dramatic reduction of a predicted maximum NS mass, if one uses the universal scaling for masses of all mesons.Nevertheless, the NS maximum mass still passes the observational constraint.We have shown that limiting the decrease of the ρ-meson effective mass allow to reduce the effect of the phase transition on the EoS and increase the maximum neutron star mass.In addition, we demonstrated that our choice of the η ρ ( f ) scaling function maximizes the neutron star maximum mass in the case without ρ − condensation.With the condensate included with the universal mass scaling, the maximum mass is almost independent of the choice of η ρ ( f ).This happens because if the scaling function is chosen to minimize the effect of the ρ − condensate, the ∆ abundance is increased, and vice versa.However, this effect proves to be accidental and does not manifest itself for a different ρ meson mass scaling.

( 3 )
0 and ρ c fields.The first one is the traditional solution with only ρ (3) 0 being non-zero.The second solution is

Figure 1 .
Figure 1.Left panel: Particle fractions together with the scalar field f as functions of the total baryon density n in the BEM for the MKVOR*H∆φρ model.Only the energetically favorable regions of the solutions' branches are shown.Middle panel: The pressure as a function of the density for MKVOR*H∆φ and MKVOR*H∆φρ models.The short vertical dash shows the critical density for the 2nd order phase transition (PT).The vertical line in the left and middle panels denotes the density, at which the ρ-condensed phase becomes energetically more favorable than the normal one.Right panel: NS mass as a function of the central density for the same models as in the middle panel.Vertical dashes denote boundaries of the Maxwell construction region (shown by the dotted line), where no stable NS configurations exist.The horizontal stripe denotes the observational constraint M max ≥ (2.01 ± 0.04) M [2] and large dots denote the maximum masses for the models.