Shedding Light on the EOSGravity Degeneracy and Constraining the Nuclear Symmetry Energy from the Gravitational Binding Energy of Neutron Stars
Abstract
A thorough understanding of properties of neutron stars requires both a reliable knowledge of the equation of state (EOS) of superdense nuclear matter and the strongfield gravity theories simultaneously. To provide information that may help break this EOSgravity degeneracy, we investigate effects of nuclear symmetry energy on the gravitational binding energy of neutron stars within GR and the scalartensor subset of alternative gravity models. We focus on effects of the slope of nuclear symmetry energy at saturation density and the highdensity behavior of nuclear symmetry energy. We find that the variation of either the density slope or the highdensity behavior of nuclear symmetry energy leads to large changes in the binding energy of neutron stars. The difference in predictions using the GR and the scalartensor theory appears only for massive neutron stars, and even then is significantly smaller than the difference resulting from variations in the symmetry energy.
Shedding Light on the EOSGravity Degeneracy and Constraining the Nuclear Symmetry Energy from the Gravitational Binding Energy of Neutron Stars
XiaoTao He^{a}^{a}aemail: hext@nuaa.edu.cn, F. J. Fattoyev^{b}^{b}bemail: ffattoye@indiana.edu, BaoAn Li^{c}^{c}cemail: baoan.li@tamuc.edu, and W. G. Newton^{d}^{d}demail: william.newton@tamuc.edu
1College of Material Science and Technology, Nanjing University of Aeronautics and Astronautics, Nanjing 210016, China
\@textsuperscript2Department of Physics and Astronomy, Texas A&M UniversityCommerce, Commerce, TX 75429, USA
\@textsuperscript3Center for Exploration of Energy and Matter, Indiana University, Bloomington, IN 47408, USA

Abstract.
1 Introduction
Neutron stars (NSs) are among the most compact, dense and neutronrich objects known in the Universe. The typical surface compactness parameter of NSs is of the order of , which is 5 orders of magnitudes larger than that at the surface of the sun (). If one uses instead a more natural measure of the gravitational field strength, the “curvature” parameter , which is related to the nonvanishing components of the Riemann tensor in vacuum as well as to the Kretschmann invariant outside the star, the surface curvature for a neutron star is then 14 orders of magnitudes larger than that at the surface of the Sun, where Solar System tests of General Relativity in the weak field regime are usually performed. The strong gravitational field makes NSs as good testbeds for the untested strongfield gravity regime, while their highdensity matter content make them as natural laboratories for determining the EOS of the superdense nuclear matter [1, 2, 3, 4, 5]. However, it cannot simultaneously be good testing ground for both. There is a possible degeneracy between the models of the neutronstar matter EOSs and models of gravity applied to describe their properties. How to break this degeneracy is a longstanding problem to which many recent studies have been devoted (see e.g., [6, 7, 8, 9, 10, 11, 12, 13, 14, 4, 15, 16, 17, 18, 5]). This talk is based on the work originally published in Ref. [19]. Here we present our analyses of the extent to which a EOSGravity degeneracy exists when models of gravity are limited to classical GR and ScalarTensor (ST) theories, while variations of the EOS appear as a result of variation of the slope of the nuclear symmetry energy at saturation density or the highdensity behavior of the nuclear symmetry energy. We find that the variation of either the density slope or the highdensity behavior of nuclear symmetry energy within their uncertainty ranges lead to significant changes in the binding energy of NSs. In particular, the variations are significantly greater than those that result from ST theories of gravity, leading to the conclusion that within those subset of gravity models, measurements of neutron star properties constrain mainly the EOS. Further investigations demonstrate that only EOSs with the soft symmetry energy at highdensity are consistent with constraints on the gravitational binding energy of PSR J07373039B.
2 The Equation of State of Nuclear Matter
In general, the EOS of neutronrich nucleonic matter can be expressed in terms of the binding energy per nucleon in asymmetric nuclear matter of isospin asymmetry as , where is the binding energy per nucleon in symmetric nuclear matter (), is the nuclear symmetry energy, and is the total baryon density with () being the neutron (proton) density. The EOS can further be characterized in terms of bulk nuclear properties by expanding both and in Taylor series around nuclear saturation density fm, i.e., and , where quantifies the deviations of the nuclear density from its saturation value. Terrestrial experimental nuclear data such as the ground state properties of finite nuclei and energies of giant resonances tightly constrain the binding energy at saturation and the nuclear incompressibility coefficient , hence constrain the EOS of symmetric nuclear matter . Whereas the symmetry energy at saturation is more or less known, its density slope is largely unconstrained, and the overall behavior of the symmetry energy at suprasaturation densities is quite uncertain.
For our base models we use two recently established EOSs for neutronrich nucleonic matter within the IUFSU Relativistic Mean Field (RMF) and the SkIUFSU SkyrmeHartreeFork (SHF) models [20, 21, 22]. The slope of the symmetry energy at saturation for these models is MeV. While the density dependence of symmetry energy at subsaturation densities is almost identical for these models, at suprasaturation densities of the two models give significantly different predictions of . To test the sensitivity of the gravitational binding energy of neutron stars to the variations of properties of neutronrich nuclear matter around saturation density, we have further introduced two RMF models with density slopes of the symmetry energy at saturation density of MeV and MeV. Shown in Fig. 2 are the density dependence of the symmetry energy for these four models [19].
3 Comparison of Predictions between GR & ScalarTensor Theory Using Different EOSs
Properties of neutron stars are not only sensitive to the underlying EOS, but also to the strongfield behavior of gravity. We will consider neutron stars in both GR and in the simplest natural extension of the GR known as the scalartensor theory of gravity. According to this theory, in addition to the secondrank metric tensor, , the gravitational force is also mediated by a scalar field, . The action defining this theory can be written in the most general form as [23, 24]
(1) 
where is the Ricci scalar curvature with respect to the socalled Einstein frame metric and is the scalar field potential. The physical metric is defined as . The relativistic equations for stellar structure in hydrostatic equilibrium can be written as
(2)  
(3)  
(4)  
(5)  
(6)  
where . Following the Ref. [23] we set which can only appear in models of modified gravity, and we consider a coupling function of the form [19]. For a given central pressure one can integrate the equations above from the center of the star to , where the only input required is the EOS of dense matter in chemical equilibrium. At the center of the star the Einstein frame boundary conditions are given as , while at infinity we demand cosmologically flat solution to agree with the observation . The stellar coordinate radius is determined by the condition of . The physical radius of a neutron star is found in the Jordan frame as . Notice however that the physical stellar mass as measured by an observer at infinity matches with the coordinate mass, since at infinity the coupling function approaches unity. According to the latest observational constraints the quadratic parameter of the scalartensor theory should take values of not smaller than Ref. [25, 23]. Similarly the absolute value of the linear parameter is also constrained very well by observation. We will therefore choose the upper bounds on these parameters as and [25].
In Fig. 3 we present our results for the mass versus radius relation of neutron stars as calculated by using the four EOSs discussed above both within GR and the scalartensor theory with . we observe a larger radius in the scalartensor theories than in GR only for massive neutron stars. Even so, the changes in radii are much smaller than those that arise from variation of the stiffness of the symmetry energy. In general, differences in predictions using the GR and the scalartensor theories within current observational bound on their parameters are much smaller than those due to the uncertainties in the EOS.
4 Constraining the Nuclear Symmetry Energy from the Gravitational Binding Energy
The fractional gravitational binding energy [26] [See Eqns.(2)(3)] as a function of the total gravitational mass of a neutron star is displayed in Fig. 4. Notice that in general the GR predictions give a lower absolute value of the fractional binding energy for a given NS mass then the scalartensor theory. However the difference is quite negligible compared to the uncertainties coming from the variations of the EOS. Furthermore, all lowmass NSs are indistinguishable for an observer in these two models of gravity, because the critical value for the socalled “spontaneous scalarizaton” is reached only when NSs masses exceed about solar mass. Thus measurements of NS mass and radii will lead to significantly constrain density dependence of the symmetry energy, rather than constraining gravity models within the GR and scalartensor theories.
As both the massverusradius relation and gravitational binding energy of NSs are more sensitive to different EOSs, we further examine the effects on binding energy of the uncertain symmetry energy in more details (see again Fig. 4). Notice that with the very similar lowdensity symmetry energy up to about , but different highdensity behaviors, predictions for the in the SkIUFSU and IUFSU models are quite different. This effect becomes more evident with the increase of the total gravitational mass. With the IUFSU as a reference baseline model then the relative changes in the fractional gravitational binding energies are , and for , and neutron stars respectively. This is in contrast to the predictions of the binding energy in models with soft and stiff symmetry energies at saturation—e.g., the IUFSU with MeV and the IUFSU with MeV. Again using the former as a reference model, then the relative changes in the fractional gravitational binding energies are , and for , and neutron stars respectively. Hence the fractional binding energy is more sensitive to the saturation density slope of the symmetry energy for lowmass neutron stars [27], while more sensitive to the suprasaturation behavior of the symmetry energy for massive stars [19].
The gravitational mass of the lighter pulsar PSR J07373039B is determined very accurately to be [28], which is one of the lowest reliably measured mass for any neutron star up to date. Due to its low mass it was suggested that this NS might have been formed as a result of the collapse of an electroncapture supernova from a an ONeMg white dwarf progenitor [29]. Under this assumption, it is estimated that the baryonic mass of the precollapse ONeMg core should lie between [29] and [30]. In Fig. 4 we show that only models with the soft symmetry energy are consistent with these set of constraints.
5 Summary
Interpreting properties of neutron stars require a resolution in the degeneracy between the EOS for superdense matter and the strongfield gravity. With the goal of providing information that may help break this degeneracy we have studied effects of the nuclear symmetry energy within its current uncertain range on the massversusradius relation and the binding energy of NSs within both the GR and the scalartensor theory of gravity. We have found that radii of neutron stars are primarily sensitive to the underlying EOS through the density dependence of the symmetry energy. Within the simplest natural extension of the GR known as the scalartensor theory of gravity, and by using upper observational bounds on the parameters of the theory, we found a negligible change in the binding energy of NSs over the whole mass range, and significant changes in radii only for NSs whose mass are well above . Even then, the changes in radii are found to be much smaller than those that result from variation of the stiffness of the symmetry energy. We have also shown that the gravitational binding energy is moderately sensitive to the nuclear symmetry energy, with lower mass neutron stars probing primarily the stiffness of the symmetry energy at nuclear saturation density, and massive stars being more sensitive to the high density behavior of the symmetry energy. A combination of observational and theoretical arguments on the gravitational binding energy of PSR J07373039B imply that only EOSs with soft symmetry energy at high density are consistent with the extracted values of the binding energy.
6 Acknowledgements
This work is supported in part by the National Natural Science Foundation of China under Grant No. 11275098, 11275067 and 11320101004, the US National Science Foundation under Grant No. PHY1068022 and the CUSTIPEN (ChinaU.S. Theory Institute for Physics with Exotic Nuclei) under DOE grant number DEFG0213ER42025, and DOE grants DESC0013702 (Texas A&M UniversityCommerce), DEFG0287ER40365 (Indiana University) and DESC0008808 (NUCLEI SciDAC Collaboration).
References
 [1] J.M. Lattimer, M. Prakash, Phys. Rept. 442, 109 (2007).
 [2] J.M. Lattimer, Ann. Rev. Nucl. Part. Sci. 62, 485 (2012).
 [3] B.A. Li, L.W. Chen, C.M. Ko, Phys. Rept. 464, 113 (2008).
 [4] P. Pani, E. Berti, V. Cardoso, J. Read, Phys. Rev. D84, 104035 (2011).
 [5] K.Y. Eksi, C. Gungor, M.M. Turkouglu, Phys. Rev. D89, 063003 (2014).
 [6] C.M. Will, Living Rev. Rel. 9, 3 (2006).
 [7] T. Harada, Phys. Rev. D57, 4802 (1998).
 [8] H. Sotani, K.D. Kokkotas, Phys. Rev. D70, 084026 (2004).
 [9] P.D. Lasky, H. Sotani, D. Giannios, Phys. Rev. D78, 104019 (2008).
 [10] D.H. Wen, B.A. Li, L.W. Chen, Phys. Rev. Lett. 103, 211102 (2009).
 [11] A. Cooney, S. DeDeo, D. Psaltis, Phys. Rev. D82, 064033 (2010).
 [12] M. Horbatsch, C. Burgess, JCAP 1108, 027 (2011).
 [13] A.S. Arapoglu, C. Deliduman, K.Y. Eksi, JCAP 1107, 020 (2011).
 [14] C. Deliduman, K. Eksi, V. Keles, JCAP 1205, 036 (2012).
 [15] H. Sotani, Phys. Rev. D86, 124036 (2012).
 [16] W. Lin, B.A. Li, L.W. Chen, D.H. Wen, J. Xu, J. Phys. G41, 075203 (2014).
 [17] K. Yagi, L.C. Stein, N. Yunes, T. Tanaka, Phys.Rev. D87, 084058 (2013).
 [18] H. Sotani, Phys. Rev. D89, 104005 (2014).
 [19] X.T. He, F.J. Fattoyev, B.A. Li, W.G. Newton, Phys. Rev. C91, 015810 (2015).
 [20] F.J. Fattoyev, C.J. Horowitz, J. Piekarewicz, G. Shen, Phys. Rev. C82, 055803 (2010).
 [21] F.J. Fattoyev, W.G. Newton, J. Xu, B.A. Li, Phys. Rev. C86, 025804 (2012).
 [22] F.J. Fattoyev, J. Carvajal, W. Newton, B.A. Li, Phys.Rev. C87, 015806 (2013).
 [23] T. Damour, G. EspositoFarese, Phys.Rev. D54, 1474 (1996).
 [24] S.S. Yazadjiev, D.D. Doneva, K.D. Kokkotas, K.V. Staykov, JCAP 1406, 003 (2014).
 [25] P.C. Freire, N. Wex, G. EspositoFarese, J.P. Verbiest, M. Bailes et al., Mon.Not.Roy.Astron.Soc. 423, 3328 (2012).
 [26] S. Weinberg, Gravitation and Cosmology (John Wiley & Sons, New York, 1972)
 [27] W. Newton, B.A. Li, Phys.Rev. C80, 065809 (2009).
 [28] M. Kramer, I.H. Stairs, R. Manchester, M. McLaughlin, A. Lyne et al., Science 314, 97 (2006).
 [29] P. Podsiadlowski, J. Dewi, P. Lesaffre, J. Miller, W. Newton et al., Mon.Not.Roy.Astron.Soc. 361, 1243 (2005).
 [30] F. Kitaura, H.T. Janka, W. Hillebrandt, Astron.Astrophys. 450, 345 (2006).