(No) neutron star maximum mass constraint from hypernuclei
Abstract
 Background

The recently accurate measurement of the mass of two pulsars close to or above has raised the question whether such large pulsar masses allow for the existence of exotic degrees of freedom, such as hyperons, inside neutron stars.
 Purpose

In the present work we will investigate how the existing hypernuclei properties may constrain the neutron star equation of state and confront the neutron star maximum masses obtained with equations of state calibrated to hypernuclei properties with the astrophysical constraint.
 Method

The study is performed using a relativistic mean field approach to describe both the hypernuclei and the neutron star equations of state. Unified equations of state are obtained. A set of five models that describe when only nucleonic degrees of freedom are employed. Some of these models also satisfy other well established laboratory or theoretical constraints.
 Results

The meson couplings are determined for all the models considered, and the potential in symmetric nuclear matter and matter at saturation are calculated. Maximum neutron star masses are determined for two values of the meson coupling, and , and a wide range of values for . Hyperonic stars with the complete baryonic octet are studied, restricting the coupling of the and hyperons to the , and mesons due to the lack of experimental data, and maximum star masses calculated.
 Conclusions

We conclude that the currently available hypernuclei experimental data and the lack of constraints on the asymmetric equation of state of nuclear matter at high densities do not allow to further constrain the neutron star matter equation of state using the recent observations. It is shown that the potential in symmetric nuclear matter takes a value MeV at saturation for the coupling given by the SU(6) symmetry, being of the order of the values generally used in the literature. On the other hand, the potential in matter varies between 16 and 8 MeV taking for vector mesons couplings the SU(6) values, at variance with generally employed values between and MeV. If the SU(6) constraint is relaxed and the vector meson couplings to hyperons is kept to values not larger than to nucleons then values between and MeV are obtained.
I Introduction
Neutron stars are among the smallest and densest objects in the Universe. With radii of the order of km and masses that can be at least as large as two solar masses, matter inside neutron stars is subject to extreme conditions of density, isospin asymmetry and magnetic field intensities. These objects constitute perfect laboratories to study nuclear matter under extreme conditions and the QCD phase diagram at low temperatures and high densities, and, therefore, they have been attracting the attention of different fields of physics. Traditionally neutron star matter has been modelled as a uniform neutronrich fluid in equilibrium with respect to the weak interactions (stable matter) surrounded by a nonhomogeneous crust. Neutrons in the inner crust and neutrons and protons in the uniform core of the star are expected to be superfluid. Due to the large value of the density, new degrees of freedom are expected to appear in the inner core of neutron stars in addition to nucleons. Among others, hyperons, BoseEinstein condensates of kaons or pions, or even deconfined quark matter have been considered.
Contrary to terrestrial conditions, where hyperons are unstable and decay into nucleons through weak interactions, matter in neutron stars maintains the weak equilibrium between the decays and their inverse capture processes. Since the pioneering work of Ambartsumyan and Saakyan in 1960 ambart (), the presence of hyperons in neutron stars has been studied by many authors using either microscopic micro (); vlowk (); dbhf1 (); dbhf2 (); qmc () or phenomenological rmf (); shf () approaches to the neutron star matter equation of state (EoS). All these works agree that hyperons may appear in the inner core of neutron stars at densities around ( fm) when the nucleon chemical potential is large enough to make the conversion of a nucleon into a hyperon energetically favourable. This conversion relieves the Fermi pressure exerted by nucleons making the EoS softer. Consequently the mass of the star, and, in particular, its maximum value , is substantially reduced. In microscopic calculations (see e.g., Refs. micro (); vlowk ()), this reduction can be even below the value of the mass of the Hulse–Taylor pulsar () hulsetaylor (). This is not the case, however, in phenomenological calculations which find values of compatible with the canonical value above. In fact, most relativistic mean field (RMF) models including hyperons predict maximum masses in the range rmf (), although with some parametrizations masses as large as could be even obtained bombaci08 (); cavagnoli11 ().
The presence of hyperons in neutron stars seems to be energetically unavoidable, although the strong softening of the EoS associated with their appearance (notably in microscopic models) leads to the prediction of maximum masses not compatible with observations. A natural question, therefore, arises: can hyperons still be present in the interior of neutron stars if is reduced to values not compatible with astrophysical observations, although their presence is energetically favourable? This question is at the origin of what has been called the “hyperon puzzle”. Its nontrivial solution is currently a subject of intense research, specially in view of the recent measurements of unusually high masses of the millisecond pulsars PSR J16142230 () demorest (); fonseca (), and PSR J0348+0432 () antoniadis () which ruled out almost all currently proposed EoS with hyperons. The solution of this problem demands a mechanism that could eventually provide the additional repulsion to make the EoS stiffer and the maximum mass compatible with observation fortin2015 (). Three different mechanisms have been proposed: (i) the inclusion of a repulsive hyperonhyperon interaction through the exchange of vector mesons Bednarek11 (); Weissenborn (); Oertel14 (); Maslov (), or less attractive scalar meson exchange Dalen (), at the cost of potentially making the EoS too stiff around and below saturation density and, therefore, incompatible with recent quantum Monte Carlo nuclear matter Gandolfi12 () and chiral effective field theory Hebeler13 () calculations, (ii) the inclusion of repulsive hyperonic threebody forces taka (); vidanatbf (); yamamoto (); lonardoniprl (), or (iii) the possibility of a phase transition to deconfined quark matter at densities below the hyperon threshold Ozel (); WeissenbornSagert (); Klahn2013 (); Bonanno (); Lastowiecki2012 (). An alternative way to circumvent the hyperon puzzle by invoking the appearance of other hadronic degrees of freedom such as for instance the isobar that push the onset of hyperons to higher densities has also been considered Drago (). We note that very recently, Haidenbauer et al., haidenbauer16 () have shown that the singleparticle potential, obtained in a Brueckner–Hartree–Fock calculation using a hyperonnucleon interaction derived from an SU(3) chiral effective field theory, becomes strongly repulsive for densities larger than , therefore, shifting the onset of hyperons to extremely high densities potentially solving the hyperon puzzle without the necessity of invoking any of these more exotic mechanisms.
In addition to the observation of massive neutron stars, more astrophysical constraints on the neutron star EoS, and, consequently, on its hyperon content such as the measurement of their radius, moment of inertia, or the surface gravitational redshift from spectral lines may come in the near future thanks to the next generation of Xray telescopes or radio observatories. No measurement of the two latter quantities has been obtained so far. Many techniques have been devised to determine neutron star radii but current estimates are still controversial both on theoretical and observational grounds (see e.g., discussions in fortin2015 (); Miller2016 (); Haensel2016 (). The future Xray missions such as NICER nicer (), Athena athena () and potential LOFTlike missions loft () promise simultaneous determinations of the mass and radius with a precision.
In the present work we analyse the possibility of obtaining two solar mass hyperonic stars within the relativistic mean field (RMF) approach when the hyperonmeson couplings are constrained by the existing experimental hypernuclear data. We shall consider a set of models that satisfy the two solar mass constraint imposed by the pulsars J16142230 and J0348+0432 when only purely nucleonic degrees of freedom are considered, and discuss the consequences of including hyperons when hypernuclear data is used to constrain the hyperonnucleon and the hyperonhyperon interactions. In particular, the experimental data on single and double hypernuclei will be taken into account in the model within the framework of the RMF approach as it is done in Ref. Shen06 (). Recently, a study with a similar objective has been performed in Ref. Sedrakian14 (). The authors of this work used symmetry arguments to fix the couplings of the vector mesons to hyperons and single hypernuclei binding energies to constrain the coupling of the meson to the hyperon. The coupling of the other hyperons to the meson were obtained requiring that the lower bound on the maximum mass of the star is . In this work, we follow the same procedure to fix the meson coupling but a different approach is used for the other couplings. In particular, we take also into account the experimental data on double hypernuclei. A comparison between the two approaches is presented.
The manuscript is organized in the following way. In section II we describe and summarize the main properties of the different RMF parametrizations used in this work. Then, in section III, we review the current status of available hypernuclear experimental data. In section IV, we explain how the binding energies of single and double hypernuclei are used to calibrate the coupling constants of the hyperon with the different mesons in the RMF models. We confront our results for the potential at saturation with the usual values taken in the literature and provide tables with values of the couplings calibrated to uptodate hypernuclear data. Hyperonic and unified EOS are then built in section V and their predictions for are confronted to the existence of objects. We finish by shortly summarizing our results and presenting our conclusions in section VI.
Ii RMF models
Model  Ref  

(fm)  (MeV)  (MeV)  (MeV)  (MeV)  (MeV)  ()  
TM1  0.146  16.3  281.2  36.9  111.2  33.8  2.18  TM1 () 
TM2  0.146   16.4  281.7  32.1  54.8  70.5  2.25  providencia13 () 
NL3  0.149  16.2  271.6  37.4  118.9  101.6  2.77  NL3 () 
NL3  0.148  16.2  271.6  31.7  55.5  7.6  2.75  NL3wra () 
DDME2  0.152  16.1  250.9  32.3  51.2  87.1  2.48  DDME2 () 
TM1  TM2  NL3  NL3  DDME2  
511.198  511.198  508.194  508.194  550.1238  
783  783  782.501  782.501  783  
770  770  763  763  763  
10.029  9.998  10.217  10.217  10.5396  
12.614  12.503  12.868  12.868  13.0189  
9.264  11.303  8.948  11.277  7.3672  
3.043  3.523  10.431  10.431  0  
3.710  47.362  28.885  28.885  0  
0.0169  0.0113  0  0  0  
0  0.03  0  0.03  0 
In the following, five different RMF models, all predicting purely nucleonic stars, are considered: four nonlinear Walecka type models with constant coupling parameters and one densitydependent model with coupling parameters that depend on the density. Among the first, we consider the parametrizations TM1 TM1 (), TM2 providencia13 (), NL3 NL3 () and NL3 NL3wra (), and for the latter we choose the model DDME2 DDME2 (). Some of their nuclear properties as well as their prediction for the neutron star maximum mass are presented in Table 1. In the following we briefly explain the reasons for the choice of these particular models.
The parametrization TM1 TM1 () was used in Ref. Shen06 () to describe single and double hypernuclei, and, we will consider it as a reference. This model includes a nonlinear meson term which softens the EoS at high densities and is the underlying model of the Shen–Toki–Oyamatzu–Sumiyoshi supernova EoS stosa (); stosb (). However, this EoS has a too large symmetry energy slope parameter ( MeV) and does not satisfy the subsaturation neutron matter constraints imposed by microscopic calculations Hebeler13 (). Including a nonlinear term that mixes the and mesons allows to overcome these two shortcomings. This term has been added to the TM1 parametrization, resulting in the parametrization TM2 providencia13 () that besides has a weaker nonlinear term turning the EoS stiffer than TM1 at large densities. We also consider the NL3 parametrization NL3 () which was fitted to the ground state properties of both stable and unstable nuclei. This parametrization predicts very large purely nucleonic neutron star maximum masses but has the drawback of having, as TM1 , a too large symmetry energy slope ( MeV). Thus we will also consider the parametrization NL3 NL3wra () with a softer density dependence of the symmetry energy due to inclusion of the nonlinear term. We note here that in Ref. Fortin16 () this parametrization was one of the few (only four) parametrizations chosen as satisfying a set of consensual constraints and still able of describing stars. The model DDME2 with density dependent couplings was another one of these four parametrizations which we will also choose in the present study. We note also that of these five parametrizations only TM1, TM2 and DDME2 satisfy the constraints imposed by the flow of matter in heavy ion collisions danielewicz02 () (see the discussion in Ref. Dutra14 ()). However, since the analysis of the experimental flow data is quite complex and not totally model independent, this constraint should be taken with care. Therefore, we will also consider the two parametrizations NL3 and NL3. The set of parameters of all the models is shown in Table 2. The parameters for the DDME2 model are shown at saturation density.
The inclusion of hyperons in RMF models is performed in a quite natural way gm91 (); Schaffner96 (). The hyperonnucleon (YN) interaction is described by means of the exchange of , and mesons similarly to the nucleonnucleon (NN) one. The hyperonhyperon (YY) interaction is included in our model by considering also the coupling of hyperons with the hidden strangeness mesons and . The Lagrangian density for a system that includes the eight lightest baryons, i.e., the nucleon doublet (neutron and proton ) and the six lightest hyperons (, the triplet, and the doublet), reads TM1 (); providencia13 ():
(1)  
(2)  
(3)  
(4)  
(5)  
(6)  
(7)  
(8) 
where and is the effective mass of baryon . and are the baryon and lepton Dirac fields, respectively, and is the coupling constant of meson with baryon . The mass of baryon and lepton are denoted by and , respectively. The constants , , are the couplings associated with the nonlinear interaction terms, and is the isospin operator. The mesonic field tensors are given by their usual expressions: , , and . The couplings are constant for for the models TM1, TM2, NL3 and NL3 whereas are density dependent in DDME2. We will explain latter in section IV how all these couplings are fixed. Here we simply indicate that the coupling constants of the nucleons with the and mesons are set to zero.
Iii Brief overview of hypernuclear physics
Whereas the NN interaction is fairly well known due to the large number of existing scattering data, the YN and YY ones are still poorly constrained. Experimental difficulties due to the short lifetime of hyperons and the low intensity beam fluxes have limited the number of N and N scattering events to several hundreds engelmann66 (); alexander68 (); sechi68 (); kadyk71 (); eisele71 (), and that of N events to very few. In the case of the YY interaction the situation is even worse because no scattering data exists at all. This limited amount of data is not enough to fully constrain these interactions.
In the absence of scattering data, alternative information on the YN and YY interactions can be obtained from the study of hypernuclei, bound systems composed of nucleons and one or more hyperons. Hypernuclei were discovered in 1952 with the observation of a hyperfragment in a ballonflown emulsion stack by Danysz and Pniewski dapnie52 (). Since then more than 40 single hypernuclei, and few double dl0 (); dl1 (); dl1b (); dl2 (); dl3 (); dl4 (); dl5 (); nagara () and single khaustov00 (); nakazawa15 () ones have been identified thanks to the use of highenergy accelerators and modern electronic counters. On the contrary, it has not been possible to prove without any ambiguity the existence of hypernuclei (see e.g., Refs. bertini80 (); bertini84 (); bertini85 (); piekarz82 (); yamazaki85 (); tang88 (); bart99 (); hayano89 (); nagae98 ()) which suggests that the nucleon interaction is most probably repulsive dgm89 (); batty1 (); batty2 (); batty3 (); mares95 (); dabrowski99 (); noumi02 (); saha04 (); harada05 (); harada06 ().
Single hypernuclei can be produced by several mechanisms such as: strangeness exchange reactions, where a neutron hit by a is changed into a emitting a . The analysis of these reactions showed many of the hypernuclear characteristics such as, for instance, the small spinorbit strength of the YN interaction, or the fact that the essentially retains its identity inside the nucleus. The use of beams permitted to perform associated production reactions, where an pair is created from the vacuum, and a and a are produced in the final state. The electroproduction of hypernuclei by means of the reaction provides a high precision tool for the study of hypernuclear spectroscopy hugenford94 () due to the excellent spatial and energy resolution of the electron beams. Recently, the HypHI collaboration at FAIR/GSI has proposed a new way to produce hypernuclei by using stable and unstable heavy ion beams hypHI (). The and the H and H hypernuclei have been observed in a first experiment performed using a Li beam on a C target at 2 A GeV rappold13 ().
Hypernuclei can be produced in excited states if a nucleon in a p or higher shell is replaced by a hyperon. The energy of these excited states can be released either by emitting nucleons, or, sometimes, when the hyperon moves to lower energy states, by the emission of rays. Measurements of ray transitions in hypernuclei has allowed to analyse excited levels with an excellent energy resolution. Systematic studies of single hypernuclei indicate that the N interaction is clearly attractive hashimoto06 ().
hypernuclei can also be produced by the mechanisms just described. However, as said before, there is not yet an unambiguous experimental confirmation of their existence.
To produce double hypernuclei, first it is necessary to create a through reactions like
(9) 
or
(10) 
Then, the should be captured in an atomic orbit and interact with the nuclear core producing two hyperons by means of the process
(11) 
providing about MeV of energy that is equally shared between the two ’s in most cases, leading to the escape of one or both hyperons from the nucleus. hypernuclei can be produced by means of the reactions (9) and (10) and, as said above, very few of them have been identified. The analysis of the experimental data from production reactions such as CBe kau () indicates an attractive nucleus interaction of the order of about MeV. Here we should mention the very recent observation of a deeply bound state of the N system with a binding energy of MeV by Nakazawa et al. nakazawa15 (). This event provides the first clear evidence of a deeply bound state of this system by an attractive N interaction. Future hypernuclei experiments are being planned at JPARC.
Doublestrange hypernuclei are nowadays the best systems to investigate the properties of the baryonbaryon interaction in the strangeness sector . The bond energy in double hypernuclei can be determined experimentally from the measurement of the binding energies of double and single hypernuclei as
(12) 
Emulsion experiments dl1 (); dl2 (); dl3 (); dl4 () have reported the formation of a few double hypernuclei: He, Be and B. From the subsequent analysis of these emulsion experiments a quite large bound energy of around 4 to 5 MeV was deduced, contrary to expectation from SU(3) (Stoks and Rijken 1999 in Ref. nijmegen ()). We should also note that the identification of some of these double hypernuclei was ambiguous. Therefore, careful attention should be paid when using the data from this old analysis to put any kind of constraint on the interaction. However, a new He candidate having a bond energy
(13) 
was unambiguously observed in 2001 at KEK nagara (). This value has then been recently revised due to a change in the value of the mass Ahn13 ():
(14) 
In this work we will use these two values of to constrain the coupling of the hyperon with the meson.
Iv Calibration of the meson coupling constants
Since the is an isospinsinglet it does not couple with the meson. Therefore, only the coupling constants with the and mesons should be fixed. The usual procedure to fix these couplings consists in using the SU(6) symmetry to determine the couplings of the with the vector mesons in terms of those of the nucleons
(15) 
(16) 
and the scalar mesons ones by using data derived indirectly from hypernuclei. In particular, these couplings are obtained by imposing the value of the potential in symmetric nuclear matter, , and the value of the potential in matter, , at saturation, defined respectively as:
(17) 
and
(18)  
with , , , and the meanfield values of the , , , and meson fields, respectively, and the scalar density. The quantities are the derivatives with respect to the density of the couplings and are only different from zero for models with density dependent couplings (see the discussion below). All quantities are calculated at the saturation density . Values of MeV and MeV are usually employed in the literature to determine these couplings. The first value results from the extrapolation at of the experimental binding energy of single hypernuclei, being the mass number of the hypernucleus. The second one is usually obtained from the identification and the use of a value of 5 MeV for the binding energy of two ’s. However, as pointed before, one has to be very careful when using this old experimental data.
In this work, however, we follow a different procedure. The couplings of the with the various mesons are calibrated by fitting the experimental binding energy of hypernuclei following the approach of Refs. Sugahara94 (); Shen06 (). Before we give more specific details on the calibration procedure, we should note that we have considered two different approaches to fix the hyperonmeson couplings in the case of the model DDME2. First, we use the experimental constraints and symmetry arguments to fix the magnitude of the couplings at saturation density, as done for the other models with constant couplings. Then we consider: (i) that the hyperonmeson couplings do not depend on the density, this approach is designated simply as DDME2; and (ii) we assume for the hyperon couplings the same density dependence of the nucleonic couplings, this model will be referred as DDME2D. For explicit density dependence of the couplings the interested reader is referred to Ref. DDME2 ().
Hypernuclei binding energies are obtained by solving the Dirac equations for the nucleons and the obtained from the Lagrangian density (8) using the method described in Refs. Avancini07 (); GRT (). In this approach the hypernucleus wave function is a Slater determinant and only the lowest singleparticle positive energy states are occupied. We use the relativistic mean field approximation where the meson field operators are replaced by their expectation values and negative energy states are neglected (nosea approximation). The numerical algorithm consists in the expansion of the Dirac spinors and mesonic fields in terms of the harmonic oscillator basis. Therefore, the Dirac and KleinGordon equations are transformed into matrix equations that are solved in a selfconsistent way until convergence is achieved. For an accurate description of light hypernuclei the centerofmass correction, instead of the simple correction,
(19) 
commonly used in the literature GRT (), is calculated through the expression,
(20) 
where is the expectation value of the squared total momentum and is the hypernucleus total mass. The former expectation value is calculated from the actual manybody state of the hypernucleus.
As in Ref. Shen06 () we include the tensor term
(21) 
which is important to get a weak nuclear spinorbit interaction noble80 (); jennings91 (). The spinorbit potential for single hypernuclei is the result of two opposite contributions which partially cancel out, one is the usual associated to the difference between the derivative of the scalar () and vector () central potentials and the other due to the tensor term.
Although no experimental data are available for the spinorbit splitting of hypernuclei, taking into account the tensor term, within the quark model (), causes an improvement on the quality of the overall calibration of the coupling constants.
iv.1 Single hypernuclei
For a given value of , the ratio is calibrated to reproduce the binding energies of hypernuclei in the s and pshells (see Figure 1). The experimental data used in the calibration is taken from Table IV of Ref. Gal16 (). The best value of is determined by minimizing the function:
(22) 
where and are, respectively, the values of the binding energy of a given single hypernuclei obtained experimentally and from the modelling, and is the total number of hypernuclei for which experimental data is available. Equal, or very close, values of are obtained if only heavy hypernuclei with are considered or if the denominator in Eq. (22) is replaced by the error bar on the experimental measurements of the binding energies. Similarly the calibration is hardly affected if only sshell binding energies are taken into account or if both shells are included. In Table 3 we indicate, for two different values of , the calibrated values of as well as the associated value of the potential in symmetric baryonic matter at saturation obtained from Eq. (17), for all the models considered. In this Table and in the following for each RMF parametrization we consider two values of the ratio , one corresponding to SU(6) symmetry case labelled ‘a’ and a second with labelled ‘b’, where the symmetry is broken. We note that the values of the couplings and that of in Table 3 are remarkably similar: for the a models and for the b models, and – MeV for all the models except three of them. In Figure 1 the experimental values and the theoretical ones obtained after calibration are plotted for the TM1 model with .
Model  

TM1a  2/3  0.621  30 
TM1b  1  0.892  31 
TM2a  2/3  0.624  31 
TM2b  1  0.905  36 
NL3a  2/3  0.622  31 
NL3b  1  0.894  32 
NL3a  2/3  0.622  31 
NL3b  1  0.894  32 
DDME2a  2/3  0.615  32 
DDME2b  1  0.891  35 
DDME2Da  2/3  0.621  32 
DDME2Db  1  0.896  35 
iv.2 Double hypernuclei
Model  

TM1a  0.533  11.2  5.3  0.557  14.2  5.9  
0.833  10.0  5.4  0.849  13.0  6.0  
TM1b  0.549  0.2  6.8  0.580  4.1  7.6  
0.843  2.7  6.8  0.864  1.2  7.7  
TM2a  0.547  13.5  5.9  0.567  16.0  6.4  
0.850  14.2  6.4  0.863  16.6  6.9  
TM2b  0.563  9.4  9.4  0.589  12.7  10.1  
0.859  8.2  9.8  0.877  11.4  10.5  
NL3a  0.534  9.9  5.6  0.559  13.2  6.3  
0.835  8.4  5.7  0.851  11.6  6.4  
NL3b  0.552  5.2  7.0  0.586  0.8  8.0  
0.846  9.0  7.1  0.868  4.8  8.0  
NL3a  0.534  9.4  5.5  0.560  12.8  6.2  
0.835  7.9  5.6  0.851  11.2  6.3  
NL3b  0.552  5.2  7.0  0.586  0.8  8.0  
0.846  9.0  7.1  0.868  4.8  8.0  
DDME2a  0.538  8.4  2.7  0.561  11.6  3.4  
0.828  6.2  2.7  0.843  9.4  3.4  
DDME2b  0.563  1.6  2.8  0.592  2.5  3.7  
0.844  6.6  2.8  0.864  2.6  3.7  
DDME2Da  0.535  11.9  4.1  0.555  11.7  4.0  
0.826  10.6  4.0  0.840  10.6  4.0  
DDME2Db  0.564  6.7  4.3  0.588  6.6  4.3  
0.846  3.4  4.3  0.862  3.4  4.3 
The value of the coupling constants of the to the hiddenstrangeness mesons and is calibrated using the measured bond energy of He. Figure 2 shows for the TM1a and b models (with values adjusted to single hypernuclei) lines of constant consistent with the experimental values of the bound energy of He, i.e., within the error bars defined in Eqs. (13) and (14). In particular, the continuous lines correspond to the limits of Eq. (7), and the dashed line to the upper limit of Eq. (13), the lower limit being inside the interval defined by Eq. (14). The color contours for the figures on the left side indicate the value of the potential in matter at saturation, , obtained from Eq. (18). For completeness in the figures on the right side we also plot contours for at as this is the quantity that has been used to determine the couplings e.g., in Ref. Oertel14 (). The horizontal line corresponds to the SU(6) value . We note that for most values of the ratios and , consistent with the experimental constraint from He, the value of potential, however, greatly varies and is very different from the value of MeV generally used in the literature to fix these couplings. In Table 4 we indicate the values of , , and for two choices of the ratio : the one corresponding the SU(6) symmetry, , and another one for which the symmetry is broken. The values of and have been obtained after calibrating to the lower and upper values of the He binding energy given in Eq. (14), and MeV, respectively, for our set of models. On the one hand at saturation is shown to vary from to MeV taking the SU(6) values for vector mesons couplings, and and MeV if the vector meson couplings to hyperons are imposed to be not larger than to nucleons. These ranges strongly differ from the generally employed one in the literature, i.e., between and MeV, showing that the use of such values for is inconsistent with the hypernuclei data. On the other the values of evaluated at are restricted to a smaller range: to MeV approximately. On the whole, Tables 3 and 4 provide the complete set of values of the coupling constants for the calibrated to hypernuclear data for all our parametrizations.
V Hyperonic Neutron Stars
We now explore how the calibration of the coupling constants for the hyperon to the binding energies of single and double hypernuclei affects the properties of neutron stars, in particular the maximum mass. To do so we calculate the EoS for neutron star matter. Following the work of two of the authors Fortin16 () unified EoS are built. For the outer crust we take the EoS proposed in Ref. ruester06 (), for the inner crust we perform a Thomas Fermi calculation and allow for nonspherical clusters according to GP0 (); GP () and for the core we consider the homogeneous matter EoS.
It is well know that the consequence of the inclusion of hyperons is a softening of the EOS and thus a reduction of its maximum mass compared to the purely nucleonic case. The more hyperonic species at the density corresponding to the central one of the NS with the maximum mass, the smaller the value of . Consequently, we consider two types of hyperonic models for the neutron star core: (i) a model in which in addition to the nucleons only the hyperon is present, and (ii) a second one where we allow for the appearance of all the hyperon species from the baryonic octet. The first model constitutes a “minimal hyperonic model” in the sense that only , if they appear, are present at high density and, therefore, compared to models with a richer hyperonic composition it will predict largest maximum masses. Thus it defines the upper limit on the maximum mass of an hyperonic neutron star.
For the second model, in principle a procedure similar to the one presented in the previous section for could be used to determine the couplings for and hyperons with the different mesons. However, as mentioned in section III, there is not yet an unambiguous experimental confirmation of the existence of the hypernuclei and very few hypernuclei has been observed. Hence the couplings of the meson to the and hyperons cannot be calibrated using hypernuclear data. Therefore, in this case, we fix the value of the singleparticle potentials of the and and use equations equivalent to Eq. (17) to determine these couplings. In order to explore the dependence of the neutron star maximum mass on the choice of potentials we choose a repulsive potential for the hyperons: MeV and MeV or MeV as suggested by the observations of hypernuclei khaustov00 (); Gal16 (). In addition, since double or double hypernuclei has not been observed, in this work we do not include the coupling of these hyperons with the and mesons. We adopt the SU(6) values for the couplings to vectorisoscalar mesons:
(23) 
(24) 
and assume
(25) 
for the meson taking into account the isospin properties of the different baryons.
(MeV)  MeV)  (MeV)  

0.6164  0.15  0  32.6  154.9  107.7 
0.6164  0.45  0.15  32.6  34.3  47.5 
0.6164  0.76  0.30  32.6  88.6  14.0 
Here we should mention that the authors of Ref. Sedrakian13 (); Sedrakian14 () have considered the SU(3) flavour symmetric model to fix the couplings of the hyperons to the three mesons, , , and , and have obtained for the last two the same couplings we define in Eqs. (23)(25). For the hyperon couplings they arrive at the equality
(26) 
which they complement with two extra conditions imposing that the hyperon couplings are positive and smaller than the nucleon ones Sedrakian13 (). From hypernuclei, the ratio was fixed to 0.616 Sedrakian14 () for the DDME2 model. This value of together with the relation (26) and the condition results in the following range of values for : . Using these values for the mesonhyperon coupling ratios one can determine the hyperonic potentials in symmetric nuclear matter, taking the hyperon coupling parameters constant. Although not indicated, this seems to have been the choice in Sedrakian13 (); Sedrakian14 () since Eq. (33) in Sedrakian13 () applies to constant couplings. The results are shown in Table 5. The first two lines of this table have been obtained taking the lower and upper values for the ratio . While the value of is within the expected range since was fitted to the hypernuclei properties, the potential comes very repulsive contrary to the experimental results which seem to indicate that MeV would be a reasonable value khaustov00 (); Gal16 (). Keeping now the ratio and choosing such that MeV, Eq. (26) can be used to determine . The results are shown in the last line of Table 5. One immediately sees that the potential comes out very attractive when, in fact, it is expected to be repulsive. It appears, therefore, that the constraints resulting from the SU(3) flavour symmetric model for the hyperonscalarmeson coupling constants are not compatible with a simultaneous attractive potential and a repulsive potential, and thus are in contradiction with what experiments seem to indicate, as discussed in section III.
The left panel of Figure 3 shows the maximum mass obtained when solving the TolmanOppenheimerVolkoff (TOV) equations tov () for an EoS based on the TM1a parametrization as a function of for the two types of hyperonic models mentioned before, both with couplings adjusted to single and double hypernuclei. In addition the horizontal grey line indicates the maximum mass obtained for a purely nucleonic core (see Table 2) and the arrow shows the value of corresponding to SU(6) symmetry. The right panel shows, for the TM1a model and the two values of the potential, the composition inside the core of a neutron star with a mass equal to , taking equal to its SU(6) value and couplings adjusted to MeV and to single hypernuclei.
The influence of the value of the potential for the hyperons on the maximum mass is found to be small. Indeed the are, after the , the most numerous hyperons, owing to the fact that the potential is repulsive, and the fraction of , even if they appear, is approximately one order of magnitude smaller as shown in the right panel of Figure 3. Similarly, the value of the bound energy of He hardly affects the results since very similar values of are obtained for or 0.84 MeV as indicated in Table 4. The lower bound for TM1b is very flat, showing no dependence on because the hyperons are suppressed and if present they only appear in residual quantities. As an example see the right panel of Fig. 7 where a similar choice of couplings for is considered.
The second type of hyperonic models constitutes a “maximal hyperonic model” and sets a lower limit on the neutron star maximum mass with an hyperonic EoS, since for the and hyperons the inclusion of the vector meson will bring extra repulsion even if the scalar meson is also included, due to the vector dominance at high densities. Consequently with the two types of hyperonic models we can calculate the range of neutron star maximum masses consistent with the available experimental data on hypernuclei and confront it to the astrophysical constraints on . The width of this range reflects our current uncertainty or lack of information on the YN and YY interactions.
For the TM1a model, as shown in Figure 3, can only be reached when , i.e., when the SU(6) is very strongly broken, and with the condition that only hyperons are included in the model. Therefore, this model appears to be difficult to reconcile with both astrophysical and hypernuclear data. On the opposite, as far as the TM1b model is concerned, for any value of , the maximal hyperonic model gives and the minimum one . Thus hyperonic EoS consistent with a maximum mass of and current hypernuclear data can be obtained.
A similar approach is used for the four additional parametrizations. As shown in Figure 4 for TM2a model a maximum mass of is reached if for the minimal hyperonic model. Again, as for TM1, the breaking SU(6) symmetry is required, but to a lesser extent since maximum masses stars are larger for the TM2 parametrization than for TM1 one. For the TM2b model, the maximum mass reachable for the minimal hyperonic model is always larger than : . This model is thus compatible with both hypernuclear and astrophysical data.
Very similar results are obtained when comparing the NL3 and NL3 parametrizations, shown in Figure 5. It has to be mentioned that for models a and for small in absolute value, the maximum value of the mass can not be obtained when the function of the mass in terms of the density starts decreasing, which is the very definition of the maximum mass, but when the baryon effective mass becomes equal to 0. Such cases are not plotted in Figure 5. Any model for the NL3 and NL3 parametrizations is consistent with the existence of a neutron star and they even predict the possibility of having hyperonic neutron stars with masses at least larger than .
Results for the DDME2 and DDME2D parametrizations are plotted in Figure 6. Whether hyperon couplings are densitydependent or not appears not to affect the maximum mass for the models a, while it does for the models b.
For the DDME2 parametrization, Figure 7 shows that for the model a the is the first hyperon to set in. For a density slightly larger the also appears and the fraction of electrons and decreases. However, as soon the sets in it is favoured because the repulsive coupling is one half of the coupling of the to the . Taking , the hyperon becomes disfavoured and only a small fraction at quite high densities appears in the case with only nucleons and ’s. If the other hyperons are also taken into account there is no ’s below fm.
For the DDME2D parametrization the hyperonmeson couplings are weaker than in the previous scenario, and they decrease with the density as the nucleonmeson couplings. A weaker allows a lower onset density, and since in this model the meson coupling is quite strong the sets in first, as shown in Figure 8. The hyperon sets in at a density very close to if , otherwise if its onset is shifted to quite high densities and its fraction is always below 1%. As in the case with constant couplings, as soon as the sets in the amount of the decreases steadily, since is half the corresponding coupling for the . Having more strict constraints to fix the different hyperonmeson couplings and including the strangeness hidden mesons, and , the relative abundances will certainly change, but the total amount of strangeness is less sensitive to the relative magnitude of the couplings. For instance, making the potential in nuclear matter repulsive will certainly reduce the amount of present in matter increasing the amount of the other hyperons.
Vi Summary and Conclusions
Modelling single and double hypernuclei we first calibrate the couplings for six different RMF parametrizations. The usual way of calibrating the coupling by imposing the value of the potential in symmetric baryonic matter, i.e., using MeV, appears in agreement with the binding energy of single hypernuclei in the s and pshells. Moreover, the value of that comes out of the order of when the SU(6) value for is taken is quite independent of the model considered. This is not at all the case for the calibration of the and couplings. Calibrating to the bound energy He shows that for the models a and b the potential in pure matter varies between and MeV. This is at variance with the usual values of or MeV employed in the literature, showing that these values are inconsistent with the hypernuclear data. Tables 3 and 3 provide the values of the various couplings to the calibrated to hypernuclear data.
We then proceed by constructing unified hyperonic EoS for neutron star matter. While an approach similar to the one presented for the hyperon should in principle be used for the and ones, the lack of hypernuclear experimental data does not allow us to calibrate their couplings to hypernuclei properties. Consequently, we proceed by devising two limiting hyperonic models. In the minimal one only the hyperon is included in addition to the nucleons and its couplings calibrated to hypernuclear data. The and hyperons are included in the maximal hyperonic model using a repulsive potential in symmetric baryonic matter for the and a value for of MeV consistent with the scarce experimental constraint for this hyperon. For these two hyperons no coupling to the hidden mesons and is included because of the nonexisting experimental data that would allow to constrain the coupling parameters.
Finally, we confront the EoS calibrated to hypernuclear data to the astrophysical constraint that neutron stars with exist. For the TM1 and TM2 parametrizations the breaking of the SU(6) symmetry appears required to be consistent with this constraint, and it is still not clear if even breaking the SU(6) the 2 limit is satisfied when all the hyperons of the baryonic octet also interact with the and mesons. The NL3, NL3 models predict the existence of hyperonic stars with masses larger than at least . However, these two models pose some problems due to the fact that the effective mass becomes negative at densities lower than that of the maximum mass for values of the coupling close to the SU(6) value, meaning that the models are unacceptable if future constraints indicate that the appropriate couplings lie in the range that results in a negative effective mass. The DDME2 and DDME2D models are both consistent with the constraint.
In conclusion it still appears difficult to exclude any of the parametrizations used in this work on the ground that hyperonic stars are not consistent with the existence of although our models are calibrated to uptodate hypernuclei data. This reflects the fact that the properties of the nucleonic sector are themselves hardly constrained at high density. Future measurements of neutron star properties (mass and radius, surface gravitational redshift, moment of inertia, …) and of high density properties of asymmetric nuclear matter in the laboratory appear necessary to constrain further the nucleonic EoS. If in addition properties of and hyperons are better constrained one could reduce the range of possible maximum masses given by the minimal and maximal hyperonic models, and potentially solve the hyperon puzzle.
Acknowledgements.
Partial support comes from “NewCompStar”, COST Action MP1304. The work of M.F. has been partially supported by the NCN (Poland) Grant No. 2014/13/B/ST9/02621 and by the STSM grant from the COST Action MP1304, and by Fundação para a Ciência e Tecnologia (FCT), Portugal, under the project No. UID/FIS/04564/2016.References
 (1) V. A. Ambartsumyan and G. S. Saakyan, Sov. Astron. 4, 187 (1960).
 (2) H.J. Schulze, M. Baldo, U. Lombardo, J. Cugnon and A. Lejeune, Phys. Lett. B 355 21 (1995); H.J. Schulze, M. Baldo, U. Lombardo, J. Cugnon and A. Lejeune, Phys. Rev. C 57, 704 (1998); M. Baldo, G. F. Burgio and H.J. Schulze, Phys. Rev. C 58, 3688 (1998). M. Baldo, G. F. Burgio and H.J. Schulze, Phys. Rev. C 61, 055801 (2000); I. Vidaña, A. Polls, A. Ramos, M. HjorthJensen and V. G. J. Stoks, Phys. Rev. C 61, 025802 (2000); I. Vidaña, A. Polls, A. Ramos, L. Engvik and M. HjorthJensen, Phys. Rev. C 62, 035801 (2000); HJ. Schulze, A. Polls, A. Ramos and I. Vidaña, Phys. Rev. C 73, 058801 (2006); H.J. Shulze and T. Rijken, Phys. Rev. C 84, 035801 (2011).
 (3) H. Dapo, B.J. Schaefer and J. Wambach, Phys. Rev. C 81, 035803 (2010).
 (4) F. Sammarruca, Phys. Rev. C 79 034301 (2009).
 (5) T. Katayama and K. Saito, arXiv:1410.7166 (2014); arXiv:1501.05419 (2015).
 (6) D. Lonardoni, F. Pederiva and S. Gandolfi, Phys. Rev. C 89 014314 (2014).
 (7) N. K. Glendenning, Phys. Lett. B 114, 392 (1982); N. K. Glendenning, Astrophys. J. 293, 470 (1985); N. K. Glendenning, Z. Phys. A 326, 57 (1987); N. K. Glendening and S. A. Moszkowski, Phys. Rev. Lett. 67, 2414 (1991); F. Weber and M. K. Weigel, Nucl. Phys. A 505, 779 (1989). R. Knorren, M. Prakash and P. J. Ellis, Phys. Rev. C 52, 3470 (1995); J. Schaffner and I. Mishustin, Phys. Rev. C 53, 1416 (1996); H. Huber, F. Weber, M. K. Weigel and Ch. Schaab, Int. J. Mod. Phys. E 7, 310 (1998).
 (8) S. Balberg and A. Gal, Nucl. Phys. A 625, 435 (1997); S. Balberg, I. Lichtenstadt and G. B. Cook, Astrophys. J. Suppl. Ser. 121, 515 (1999). D. E. Lanskoy and Y. Yamamoto, Phys. Rev. C 55, 2330 (1997); T. Y. Tretyakova and D. E. Lanskoy, Eur. Phys. J. A 5, 391 (1999); J. Cugnon, A. Lejeune and H.J. Schulze, Phys. Rev. C 62, 064308 (2000); I. Vidaña, A. Polls, A. Ramos and H.J. Schulze, Phys. Rev. C 64, 044301 (2001); X.R. Zhou , H.J. Schulze, H. Sagawa, C.X. Wu and E.G. Zhao, Phys. Rev. C 76, 034312 (2007); X.R. Zhou, A. Polls, H.J. Schulze and I. Vidaña, Phys. Rev. C 78, 054306 (2008).
 (9) R. A. Hulse and J. H. Taylor, Astrophys. J. Lett. 195 L51 (1975).
 (10) I. Bombaci, P. K. Panda, C. Providência, and Isaac Vidaña, Phys. Rev. D 77, 083002 (2008)
 (11) R. Cavagnoli, D. P.Menezes and C. Providência, Phys. Rev. C 84, 065810 (2011)
 (12) P. Demorest et al., Nature 467, 1081 (2010).
 (13) Fonseca, E., Pennucci, T. T., Ellis, J. A., et al. 2016, arXiv:1603.00545
 (14) J. Antoniadis et al., Science 340 6131 (2013).
 (15) M. Fortin, J. L. Zdunik, P. Haensel and M. Bejger, Astron. and Astrophys. 576, A68 (2015).
 (16) I. Bednarek, P. Haensel, J. L. Zdunik, M. Bejger and R. Mańka, Astron. and Astrophys. 543, A157 (2012).
 (17) S. Weissenborn, D. Chatterjee, and J. Schaffner–Bielich, Phys. Rev. C 85, 065802 (2012).
 (18) M. Oertel, C. Providência, F. Gulminelli and Ad. R. Raduta, J. Phys. G. 42 075202 (2015).
 (19) K. A. Maslov, E. E. Kolomeitsev and D. N. Voskresensky, Phys. Lett. B 748 369 (2015).
 (20) E. N. E. van Dalen, G. Colucci and A. Sedrakian, Phys. Lett. B 734, 383 (2014).
 (21) S. Gandolfi, J. Carlson and S. Reddy, Phys. Rev. C 85, 032801 (2012).
 (22) K. Hebeler, J. M. Lattimer, C. J. Pethick, and A. Schwenk, ApJ 773, 11 (2013).
 (23) T. Takatsuka et al., Eur. Phys. J. A 13, 213 (2002); Prog. Theor. Phys. Suppl. 174, 80 (2008).
 (24) I. Vidaña, D. Logoteta, C. Providência, A. Polls and I. Bombaci, Eur. Phys. Lett. 94, 11002 (2011).
 (25) Y. Yamamoto, T. Furumoto, B. Yasutake and Th. A. Rijken, Phys. Rev. C 88 022801 (2013); Phys. Rev. C 90 045805 (2014).
 (26) D. Lonardoni, A. Lovato, S. Gandolfi and F. Pederiva Phys. Rev. Lett. 114 092301 (2015).
 (27) F. Özel, D. Psaltis, S. Ransom, P. Demorest and M. Alford, Astrophys. J. Lett. 724 L199 (2010).
 (28) S. Weissenborn, I. Sagert, G. Pagliara, M. Hempel and J. SchaeffnerBielich, Astophys. J. Lett. 740 L14 (2011).
 (29) T. Klähn, D. Blaschke and D. Lastowiecki, Phys. Rev. D 88 085001 (2013).
 (30) L. Bonanno and A. Sedrakian, Astron. and Astrophys. 539 416 (2012).
 (31) R. Lastowiecki, D. Blaschke, H. Grigorian and S. Typel Acta Phys. Polon. Suppl., 5 535 (2012).
 (32) A. Drago, A. Lavagno, G. Pagliara and D. Pigato, Phys. Rev. C 90, 065809 (2014); EPJ Web Conf. 95, 01011 (2015).
 (33) J. Haidenbauer, U.G. Meissner, N. Kaiser and W. Weise, arXiv:1621.03758v1 (2016).
 (34) M. C. Miller and F. K. Lamb, Eur. Phys. J. A 52, no. 3, 63 (2016)
 (35) Haensel, P., Bejger, M., Fortin, M., Zdunik, J.L. 2016, Eur. Phys. J. A 52, 59
 (36) K. C. Gendreau, Z. Arzoumanian and T. Okajima, Proc. SPIE, 8443 (2012).
 (37) C. Motch, J. Wilms, D. Barret et al. , arXiv:1306.2334 (2013).
 (38) M. Feroci, J. W. den Herder, E. Bozzo et al. Proc. SPIE 8443 (2012).
 (39) H. Shen, F. Yang, H. Toki, Prog. Theor. Phys. 115, 325 (2006).
 (40) van Dalen, E. N. E., Colucci, G., & Sedrakian, A. 2014, Physics Letters B, 734, 383
 (41) Y. Sugahara, and H. Toki, Nucl. Phys. A, 579, 557 (1994).
 (42) C. Providência and Aziz Rabhi, Phys. Rev. C 87, 055801 (2013).
 (43) G. A. Lalazissis, J. König, and P. Ring, Phys. Rev. C 55, 540 (1997).
 (44) C. J. Horowitz, and J. Piekarewicz, Phys. Rev. Lett. 86, 5647 (2001).
 (45) G. A. Lalazissis, T. Nikšić, D. Vretenar, and P. Ring, Phys. Rev. C 71, 024312 (2005).
 (46) H. Shen, H. Toki, K. Oyamatsu, and K. Sumiyoshi, Nucl. Phys. A 637, 435 (1998).
 (47) H. Shen, H. Toki, K. Oyamatsu, and K. Sumiyoshi, Astrophys. J. Suppl. 197, 20 (2011).
 (48) Fortin, M., Providência, C., Raduta, A. R., et al. 2016, Phys. Rev. C, 94, 035804
 (49) P. Danielewicz, R. Lacey, W.G. Lynch, Science 298, 1592 (2002).
 (50) M. Dutra, O. Lourenço, S. S. Avancini, et al., Phys. Rev. C 90, 055203 (2014).
 (51) N. K. Glendenning and S. A. Moszkowski, Phys. Rev. Lett. 67, 2414 (1991).
 (52) J. Schaffner and I. N. Mishustin, Phys. Rev. C 53, 1416 (1996)
 (53) R. Engelmann et al., Phys. Lett. 21, 587 (1966).
 (54) G. Alexander et al., Phys. Rev. 173, 1452 (1968)
 (55) B. Sechi–Zor et al., Phys. Rev. 175, 1735 (1968).
 (56) J. A. Kadyk et al., Nucl. Phys. B 27, 13 (1971).
 (57) J. Eisele et al., Phys. Lett. B 37, 204 (1971).
 (58) M. Danysz and J. Pniewski, Phil. Mag. 44, 348 (1953).
 (59) M. Danysz et al., Phys. Rev. Lett. 11, 29 (1963).
 (60) M. Danysz et al., Nucl. Phys. A 49, 121 (1963).
 (61) R. H. Dalitz, D. H. Davis, P. H. Fowler, A. Montwill, J. Pniewski and J. A. Zakrewski, Proc. Roy. Soc. London, Ser. A 426, 1 (1989).
 (62) D. J. Prowse, Phys. Rev. Lett. 17, 782 (1966).
 (63) S. Aoki et al., Prog. Theor. Phys. 85, 1287 (1991).
 (64) C. B. Dover, D. J. Millener, A. Gal and D. H. Davis, Phys. Rev. C 44, 1905 (1991).
 (65) G. B. Franklin, Nucl. Phys. A 585, 83c (1995).
 (66) H. Takahashi et al., Phys. Rev. Lett. 87, 212502 (2001).
 (67) P. Khaustov et al., Phys. Rev. C 61, 054603 (2000).
 (68) K. Nakazawa et al., Prog. Theor. Exp. Phys., 0033D02 (2015).
 (69) R. Bertini et al., Phys. Lett. B 90, 375 (1980).
 (70) R. Bertini et al., Phys. Lett. B 136, 29 (1984).
 (71) R. Bertini et al., Phys. Lett. B 158, 19 (1985).
 (72) H. Piekarz et al., Phys. Lett. B 110, 428 (1982).
 (73) T. Yamazaki et al., Phys. Rev. Lett. 54, 102 (1985).
 (74) L. Tang et al., Phys. Rev. C 38, 846 (1988).
 (75) S. Bart et al., Phys. Rev. Lett. 83, 5238 (1999).
 (76) R. Hayano et al., Phys. Lett. B 231, 355 (1989).
 (77) T. Nagae et al., Phys. Rev. Lett. 80, 1605 (1998).
 (78) C. B. Dover, D. J. Millener and A. Gal, Phys. Rep. 184, 1 (1989).
 (79) C. J. Batty, E. Friedman and A. Gal, Phys. Lett. B 335, 273 (1994).
 (80) C. J. Batty, E. Friedman and A. Gal, Prog. Theor. Phys. Suppl. 117, 227 (1994).
 (81) C. J. Batty, E. Friedman and A. Gal, Phys. Rep. 287, 385 (1997).
 (82) J. Mareš, E. Friedman, A. Gal and B. K. Jennings, Nucl. Phys. A 594, 311 (1995).
 (83) J. Da̧browski, Phys. Rev. C 60, 025205 (1999).
 (84) H. Noumi et al., Phys. Rev. Lett. 89, 072301 (2002); Erratum: Phys. Rev. Lett. 90, 049903(E) (2003).
 (85) P. K. Saha et al., Phys. Rev. C 70, 044613 (2004).
 (86) T. Harada and Y. Hirabayashi, Nucl. Phys. A 759, 143 (2005).
 (87) T. Harada and Y. Hirabayashi, Nucl. Phys. A 767, 206 (2006).
 (88) E. V. Hungerford, Prog. Theor. Phys. Suppl. 117, 135 (1994).
 (89) S. Bianchin et al., Int. J. Mod. Phys. E 18, 2187 (2009).
 (90) C. Rappold et al., Nucl. Phys. A 913, 170 (2013).
 (91) O. Hashimoto and H. Tamura, Prog. Part. Nucl. Phys. 57, (2006) 564.
 (92) P. Khaustov et al., Phys. Rev. C 61, (2000) 054603.
 (93) P. M. M. Maesen, T. A. Rijken, and J. J.de Swart, Phys. Rev. C 40, (1989) 2226; T. A. Rijken, V. G. J. Stoks, and Y. Yamamoto, Phys. Rev. C 59, (1999) 21; V. G. J. Stoks and T. A. Rijken, Phys. Rev. C 59, (1999) 3009; T. A. Rijken, Phys. Rev. C 73, (2006) 044007; T. A. Rijken and Y. Yamamoto, Phys. Rev. C 73, (2006) 044008.
 (94) Ahn, J. K., Akikawa, H., Aoki, S., et al. 2013, Phys. Rev. C, 88, 014003
 (95) Sugahara, Y., & Toki, H. 1994, Progress of Theoretical Physics, 92, 803
 (96) S.S. Avancini, J.R. Marinelli, D.P. Menezes, M.M.W. Moraes, A.S. Schneider, Phys. Rev. C 76, 064318 (2007).
 (97) Y. K. Gambhir, P. Ring and A. Thimet, Ann. Phys. 198 132 (1990).
 (98) J.V.Noble, Phys. Lett. 89B, 325 (1980).
 (99) M. Chiapparini, A. O. Gattone, and B. K. Jennings, Nucl.Phys. A529, 589 (1991).
 (100) Gal, A., Hungerford, E. V., & Millener, D. J. 2016, Reviews of Modern Physics, 88, 035004
 (101) S. B. Rüster, M. Hempel and J. SchaffnerBielich, Phys. Rev. C 73, 035804 (2006).
 (102) F. Grill, C. Providência, and S. S. Avancini, Phys. Rev. C 85, 055808 (2012).
 (103) F. Grill, H. Pais, C. Providência, I. Vidaña, and S. S. Avancini, Phys. Rev. C 90, 045803 (2014).
 (104) G. Colucci and A. Sedrakian, Phys. Rev. C 87, 055806 (2013).
 (105) J. R. Oppenheimer and G. M. Volkoff, Phys. Rev. 55, 374 (1939); R. C. Tolman, ibid. 55, 364 (1939).