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Key factor for determining relation between radius and tidal deformability of neutron stars: Slope of symmetry energy

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1. Li, M., Ding, W.-B., Wei, J.-M. et al. E®ects of free parameterized TOV equations on properties of neutron stars with hyperons[J]. International Journal of Modern Physics E, 2024. doi: 10.1142/S0218301324500174
2. Pradhan, B.K., Chatterjee, D., Gandhi, R. et al. Role of vector self-interaction in neutron star properties[J]. Nuclear Physics A, 2023. doi: 10.1016/j.nuclphysa.2022.122578
3. Xie, W.-J., Chen, J.-L., Ma, Z.-W. et al. Dependence of the tidal deformability of neutron stars on the nuclear equation of state[J]. Chinese Physics C, 2023, 47(1): 014103. doi: 10.1088/1674-1137/ac9888
4. Lourenço, O., Lenzi, C.H., Frederico, T. et al. Dark matter effects on tidal deformabilities and moment of inertia in a hadronic model with short-range correlations[J]. Physical Review D, 2022, 106(4): 043010. doi: 10.1103/PhysRevD.106.043010
5. Ghosh, S., Chatterjee, D., Schaffner-Bielich, J. Imposing multi-physics constraints at different densities on the neutron Star Equation of State[J]. European Physical Journal A, 2022, 58(3): 37. doi: 10.1140/epja/s10050-022-00679-w
6. Morawski, F., Bejger, M. Neural network reconstruction of the dense matter equation of state derived from the parameters of neutron stars[J]. Astronomy and Astrophysics, 2020. doi: 10.1051/0004-6361/202038130

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Nai-Bo Zhang, Bin Qi and Shou-Yu Wang. The key factor to determine the relation between radius and tidal deformability of neutron stars: slope of symmetry energy[J]. Chinese Physics C. doi: 10.1088/1674-1137/44/6/064103
Nai-Bo Zhang, Bin Qi and Shou-Yu Wang. The key factor to determine the relation between radius and tidal deformability of neutron stars: slope of symmetry energy[J]. Chinese Physics C.  doi: 10.1088/1674-1137/44/6/064103 shu
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Received: 2019-12-09
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Key factor for determining relation between radius and tidal deformability of neutron stars: Slope of symmetry energy

    Corresponding author: Shou-Yu Wang, sywang@sdu.edu.cn
  • Shandong Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment, School of Space Science and Physics, Institute of Space Sciences, Shandong University, Weihai 264209, China

Abstract: The constraints on tidal deformability Λ of neutron stars were first extracted from GW170817 by LIGO and Virgo Collaborations. However, the relationship between the radius R and tidal deformability Λ is still under debate. Using an isospin-dependent parameterized equation of state (EOS), we study the relation between R and Λ and its dependence on parameters of symmetry energy Esym and EOS of symmetric nuclear matter E0 when the mass is fixed at 1.4 M, 1.0 M, and 1.8 M. We find that, although the changes of high order parameters of Esym and E0 can shift individual values of R1.4 and Λ1.4, the R1.4Λ1.4 relation remains approximately at the same fitted curve. The slope L of the symmetry energy plays the dominant role in determining the R1.4Λ1.4 relation. By investigating the mass dependence of the RΛ relation, we find that the well fitted RΛ relation for 1.4 M is broken for massive neutron stars.

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    1.   Introduction
    • The equation of state (EOS) of dense neutron-rich matter plays a dominant role in determining the properties of neutron stars. In turn, observations of neutron stars can place strict constraints on the EOS. Currently, the most widely used observation to constrain the EOSs is the maximum observed mass of pulsars J1614-2230 with mass M=1.908±0.016 M [1, 2] and J0348+0432 with M=2.01±0.04 M [3]. Many soft EOSs, which cannot support such high mass have been excluded. Recently, the newly reported pulsar J0740+6620 with M=2.14+0.100.09 M [4] introduced a new theoretical challenge in satisfying the constrained pressure band for several typical microscopic nuclear EOSs with maximum mass Mmax>2.14 M [5].

      Except for the mass, the radius of neutron stars is another observable that constrains the EOSs. To extract the radii, special attention is given to the quiescent low-mass X-ray binaries [6, 7] or the isolated cooling neutron stars [8], and various analyses have been performed [918]. However, due to the significant difficulties in e.g., determining the precise distance of the source and compositions of atmosphere, large uncertainties still exist, and additional information is required to estimate the correct radii (see, e.g., Refs. [12, 1922] for recent reviews).

      The first joint gravitational and electromagnetic observation of GW170817 initiated the era of multimessenger astronomy [23, 24] and further motivated an abundance of studies on the EOS in both astrophysics and nuclear physics communities (see, e.g., Refs. [25-28] for recent reviews). In a coalescing binary neutron star system, one neutron star suffers tidal deformation induced by the strong tidal field of its companion. The corresponding tidal deformability can be extracted by different methods. The dimensionless tidal deformability of the canonical neutron stars was first extracted [23] and then refined as Λ1.4=190+390120 at 90% confidence level by assuming that both neutron stars are described by the same EOS and spin at low-spin prior [29]. Considering the maximum observed mass of PSR J0348+0432, Ref. [30] improved the lower limit of Λ1.4>120 based on a generic family of neutron-star-matter EOSs that interpolate between theoretical results at low and high baryon density. Similarly, Ref. [31] modified the lower limits as Λ1.4>290 (35.5) at 3σ for neutron stars without (with) phase transition. Thereafter, various constraints have been placed on the properties of nuclei and neutron stars, such as the neutron-skin thickness of 208Pb [32-34], radius R [2933, 3543], and maximum mass Mmax [44-51] of neutron stars.

      As the dimensionless tidal deformability Λ is related to radius R by Λ=2k2/3(c2R/GM)5 [52, 53] where k2 is the second Love number, an underlying relation may exist between Λ and R when the mass is fixed. If the relation is explicit, one quantity can be extracted when the other is measured/determined. However, as the k2 is solved by a complicated differential equation coupled to TOV equations [54, 55], the exact relation between the radius and tidal deformability of canonical neutron stars (R1.4Λ1.4 relation) is still not well determined. The R1.4Λ1.4 relation has been fitted in Refs. [30, 32, 33, 35, 3739, 5658] based on the EOSs calculated from relativistic mean field (RMF) theory, Skyrme Hartree-Fock (SHF) theory, microscopic theories, or parameterized EOSs, which are summarized in Fig. 1. We observe that, though all fitted equations are found within a narrow band in the R1.4Λ1.4 plane, the uncertainty remains.

      Figure 1.  (color online) Tidal deformability Λ1.4 as a function of radius R1.4 of canonical neutron stars based on isospin-dependent parameterized EOS. Parameters L, Ksym, Jsym, and J0 are valued in steps of 5, 50, 100, and 50 MeV within their uncertainties, respectively. The horizontal dashed lines represent the refined constraints of 70<Λ1.4<580 (90% confidence level) extracted by LIGO and Virgo Collaborations [29]. Red dots labeled by the coordinates represent the constrained upper and lower limits on R1.4. Solid lines correspond to the fitted equations suggested by different studies.

      In the present study, we focus on two approaches regarding the relation between radius and tidal deformability: (1) Delineating the dependence of the R1.4Λ1.4 relation on the parameters of nuclear matter based on an isospin-dependent parameterized EOS; (2) Revealing the mass dependence of RΛ relation. The theoretical framework is summarized in Section 2. The discussion on the R1.4Λ1.4 relation and its dependence on EOS parameters and mass is presented in Section 3, and the conclusions are provided in Section 4.

    2.   Theoretical framework
    • Recently, the study in Ref. [59] constructed an isospin-dependent parameterized EOS describing the neutron stars with a core consisting of a neutron, proton, electron, and muon at β-equilibrium (charge neutral npeμ matter) and developed a numerical technique of inverting the TOV equations to constrain the EOS and symmetry energy based on the observations of radius, tidal deformability, and maximum mass, or physical requirement, such as the causality condition (speed of sound is lower than speed of light) [5, 51, 60]. The construction and demonstration are presented in detail in Ref. [59]. For completeness and ease of discussion, we first summarize the key aspects of the model. An EOS is mainly determined by the EOS of asymmetric nucleonic matter Eb(ρ,δ) with isospin asymmetry δ=(ρnρp)/ρ at density ρ through ϵ(ρ,δ)=ρ[Eb(ρ,δ)+MN]+ϵl(ρ,δ), and Eb(ρ,δ) is thus approximated as [61]

      Eb(ρ,δ)=E0(ρ)+Esym(ρ)δ2,

      (1)

      where E0(ρ) is the EOS of symmetric nuclear matter (SNM), and Esym is the symmetry energy. We parameterize E0(ρ) and Esym(ρ) as

      E0(ρ)=E0(ρ0)+K02(ρρ03ρ0)2+J06(ρρ03ρ0)3,

      (2)

      Esym(ρ)=Esym(ρ0)+L(ρρ03ρ0)+Ksym2(ρρ03ρ0)2+Jsym6(ρρ03ρ0)3,

      (3)

      using the saturation density of SNM ρ0, the incompressibility K0 and skewness J0 of SNM, as well as the slope L, curvature Ksym, and skewness Jsym of the symmetry energy.

      The above equations have the same form as the widely used Taylor expansions around ρ0. With increasing density, the convergence problem appears for Taylor expansions. However, as demonstrated in great detail in Ref. [59], the above equations can still be used to simulate nuclear matter at high density if we see the coefficients as free parameters that should be determined by the observations. The parameterizations (2) and (3) naturally become Taylor expansions when ρρ0. As free parameters, in principle, they can be varied. In this case, it is infeasible to perform a study with seven free parameters. To reduce the freedom of parameters, we first fixed the well constrained parameters as their currently known most probable values around ρ0 extracted from terrestrial nuclear laboratory experiments, namely, E0(ρ0)=15.9 MeV [62], Esym(ρ0)=31.7 MeV [63-65], and K0=230 MeV [66, 67]. As the uncertainty of L is constrained as 58.7±28.1 MeV [6365] but J0, Ksym, and Jsym are less constrained (800J0400 MeV, 400Ksym100 MeV, and 200Jsym800 MeV) [68, 69], we fixed L=58.7 MeV and studied how the observations of maximum observed mass Mmax, radius R1.4, and tidal deformability Λ1.4 of canonical neutron stars, as well as the causality condition can constrain the EOS and symmetry energy in the three-dimensional KsymJsymJ0 parameter space [51]. We found that J0, and thereby E0, have slight effects on the radius and tidal deformability of canonical neutron stars. Then, the effects of the symmetry energy on the properties of neutron stars were delineated in the three-dimensional LKsymJsym parameter space [60]. In the present study, the overall effects of LKsymJsymJ0 parameters on R1.4, Λ1.4, and the R1.4Λ1.4 relation are discussed. To enlarge the samples of EOSs, the parameter combinations are adopted within the whole parameter space constrained by experiments and theories mentioned above, and thus the causality condition is not considered in the present study.

      Using the parameterized EOS to describe the core of neutron stars, the outer and inner crusts are replaced by BPS [70] and NV EOSs [71], where the transition density is self-consistently calculated by investigating the incompressibility [72-75]:

      Kμ=ρ2d2E0dρ2+2ρdE0dρ+δ2[ρ2d2Esymdρ2+2ρdEsymdρ2E1sym(ρdEsymdρ)2].

      (4)

      Once the Kμ becomes negative, the thermodynamical instability grows by forming clusters, indicating a transition from the uniform core to the clustered crust. Notably, the crust EOSs have little effect on the maximum mass and tidal deformability [76, 77]. However, the crust EOSs have an apparent effect on the radius, e.g., in Ref. [76, 78]. The main purpose of the present study is to investigate the dependence of the RΛ relation on the core EOSs; hence, the effects of crust EOSs are not discussed.

      For a given EOS, the mass and radius can be calculated by solving the TOV equations [54, 55]:

      dPdr=G(m(r)+4πr3P/c2)(ϵ+P/c2)r(r2Gm(r)/c2),

      (5)

      dm(r)dr=4πϵr2,

      (6)

      and the tidal deformability can be obtained by solving a complicated differential equation coupled to TOV equations [52, 53].

    3.   Relation between radius and tidal deformability of neutron stars
    • The radius of neutron stars is sensitive to the symmetry energy at around two times the saturation density [79, 80]. The dependence of Λ1.4 on symmetry energy was first discussed in Refs. [81, 82], where the authors concluded that the tidal deformability of low mass neutron stars is only sensitive to the slope L of the symmetry energy, while the tidal deformability of massive neutron stars is sensitive to the high density behavior of symmetry energy. Recently, Ref. [57] studied the relation between Λ1.4 and the parameters of symmetry energy Esym and EOS of SNM E0 based on more than 200 Skyrme EOSs and found a strong relationship between Λ1.4 and the curvature Ksym of symmetry energy. Ref. [83] found that R1.4 is almost independent of L with respect to the constraints from the chiral effective field theory.

      In several previous studies, we showed the individual results of R1.4 and Λ1.4 in the three-dimensional parameter space of KsymJsymJ0 by fixing L=58.7 MeV [51, 59] and LKsymJsym by fixing J0=180 MeV [60]. We found that the slope L and curvature Ksym of the symmetry energy play almost equally important roles in determining the individual values of R1.4 and Λ1.4. To further clarify the R1.4Λ1.4 relation and its dependence on the symmetry energy and EOS of SNM, the tidal deformability Λ1.4 as a function of radius R1.4 of canonical neutron stars based on the isospin-dependent parameterized EOS is depicted by black dots in Fig. 1. The parameters L, Ksym, Jsym, and J0 are valued in steps of 5, 50, 100, and 50 MeV within their uncertainties, respectively. The horizontal dashed lines depict the refined constraints of 70<Λ1.4<580 (90% confidence level) extracted by LIGO and Virgo Collaborations [29]. The red dots labeled by the coordinates represent the constrained upper and lower limits of R1.4. The solid lines correspond to the equations fitted by other studies mentioned in the introduction. We see that almost all fitted equations are represented by present calculations, except the one from Ref. [32], where only EOSs with R1.4>12.5 km are adopted to fit the equation and the R1.4Λ1.4 relation is extrapolated with larger errors for smaller radii. Thus, the parameterized EOSs are sufficient to study the R1.4Λ1.4 relation. Considering the constraint of tidal deformability, as labeled by red dots, the radius can be constrained as 9.11<R1.4<13.14 km. This upper limit is largely consistent with Ref. [30] using EOSs interpolation between the chiral effective theory at low density and perturbative quantum chromo dynamics at high baryon density, and Ref. [84] using available terrestrial laboratory data on the isospin diffusion in heavy-ion reactions at intermediate energies. Considering the constraint of 2.01 M from Ref. [3] or the newly reported 2.14 M from Ref. [4], more parameter sets with small radii can be excluded and thus raise the lower limit of R1.4 significantly, as discussed in Ref. [30].

      As the E0(ρ) and Esym(ρ) have been parameterized in our calculations, apart from showing the overall R1.4Λ1.4 relation, the individual effects of each parameter of E0(ρ) and Esym(ρ) on the R1.4Λ1.4 relation can likewise be studied. To study the effects of Ksym and Jsym, the tidal deformability Λ1.4 as a function of radius R1.4 of canonical neutron stars when L (J0) is fixed as 30, 60, and 90 MeV (0 and 400 MeV), as shown in Fig. 2. Jsym increases from –200 to 800 MeV when Ksym is fixed at –400, –300, –200, –100, 0, and 100 MeV for each panel. Solid lines correspond to the fitted curves in the form of Λ1.4=aRb1.4. The corresponding coefficients (a, b) of the fitted equation are given in Table 1. We observe that the increase of Ksym, Jsym, or J0 can shift the data to larger Λ1.4 and R1.4 along the fitted curves for fixed L. Using the fitted curve of L=30 MeV and J0=0 MeV as a reference, the deviation between the data and fitted curve by varying Ksym and Jsym (top left panel) is less than 5%, except several points with small radii. If considering the effects of L, i.e., varying L from 30 MeV to 90 MeV (bottom left panel), the deviation increases to about 20%. Further, an additional 2% deviation is added when changing J0 from 0 to 400 MeV (bottom right panel).

      L/MeV
      30 60 90
      J0/MeV 0 (10.25, 7.040) (4.943, 7.277) (4.353, 7.283)
      400 (13.38, 6.937) (5.110, 7.268) (5.892, 7.173)

      Table 1.  Coefficients (a×106, b) of fitted equation Λ1.4=aRb1.4 for different L and J0 parameter sets given in Fig. 2, respectively.

      Figure 2.  (color online) Tidal deformability Λ1.4 as a function of radius R1.4 of canonical neutron stars when L (J0) is fixed as 30, 60, and 90 MeV (0 and 400 MeV), respectively. The Jsym is varied from –200 to 800 MeV when Ksym is fixed as –400, –300, –200, –100, 0, and 100 MeV for each plot. Solid lines correspond to the fitted curves.

      To present the above discussion more clearly, we summarize the six fitted curves in Fig. 3. The black, blue, and red lines correspond to the results of L=30, 60, and 90 MeV. The solid and dashed lines correspond to the results of J0=400 MeV and 0 MeV. We observe that although J0 changes from 400 MeV to 0 MeV, the R1.4Λ1.4 relation is almost unchanged. However, when L changes from 30 to 90 MeV, the R1.4Λ1.4 relation changes significantly. We conclude that the slope L of the symmetry energy plays the dominant role in determining the R1.4Λ1.4 relation, although L and Ksym play almost equally important roles in determining the individual values of R1.4 and Λ1.4 [60]. Thus, the precise measurement of L is crucial to determine the exact relation between R1.4 and Λ1.4, which are expected to be measured by the LIGO and Virgo Collaborations and Neutron star Interior Composition ExploreR (NICER), respectively. Notably, the exact dependence of fitted coefficients (a, b) on L is not found in the present study.

      Figure 3.  (color online) Fitted curves for different L and J0 parameter sets given in Fig. 2 with Ksym and Jsym varying within their uncertainties. Black, blue, and red lines correspond to results of L = 30, 60, and 90 MeV. The solid and dashed lines correspond to results of J0=400 and 0 MeV.

      In fact, the effects of J0 have been shown in Refs. [51, 59]. The constant surfaces of R1.4 and Λ1.4 are almost parallel to the J0 axis in the KsymJsymJ0 parameter space for L=58.7 MeV, which shows the weak dependence on J0 for R1.4 and Λ1.4, thereby the R1.4Λ1.4 relation.

      Besides, the RΛ relation is normally studied for neutron stars with M=1.4 M. To determine whether the RΛ relation still holds for low mass or massive neutron stars (e.g., R1.0Λ1.0 relation or R1.8Λ1.8 relation) requires further studies. To verify the mass dependence of the above discussions, we calculate the tidal deformability as a function of radius for neutron stars with 1.0 M (black dots), 1.4 M (red dots), and 1.8 M (blue dots) and show the results in Fig. 4. Compared to the results of neutron stars with 1.4 M, we observe that wider ranges can be covered for neutron stars with 1.0 M. This is evident, as the Λ decreases with increasing M for a given EOS (see, e.g., Ref. [60]). Moreover, as the central density of neutron stars with 1.8 M is significantly larger than that of the stars with 1.4 M, the high order parameters in Eqs. (2) and (3) start to play more important roles in determining the properties of neutron stars and thus break the well-fitted RΛ relation for canonical neutron stars.

      Figure 4.  (color online) Tidal deformability as a function of radius for neutron stars with 1.0 M (black dots), 1.4 M (red dots), and 1.8 M (blue dots) based on isospin-dependent parameterized EOS.

    4.   Summary
    • Employing an isospin-dependent parameterized EOS, we study the relation between R and Λ of neutron stars and its dependence on the symmetry energy Esym and EOS of SNM E0 when the mass is fixed at 1.4 M, 1.0 M, and 1.8 M. We find that, although the changes of high order parameters of Esym and E0 are capable of shifting the individual values of R1.4 and Λ1.4 to different values, the R1.4Λ1.4 relation remains approximately at the same fitted curve. The slope L of the symmetry energy plays the dominant role in determining the R1.4Λ1.4 relation, and the precise measurement of L is crucial to determine the exact relation between R1.4 and Λ1.4. Compared to the results of neutron stars with 1.4 M, wider ranges in the RΛ plane can be covered for neutron stars with 1.0 M and 1.8 M. Hence, the well-fitted RΛ relation for 1.4 M is broken for massive neutron stars.

      A possible relation among LR1.4Λ1.4 is found in the present study. All three relations remain inconclusive to date. Any progress on heavy-ion reactions, measurement of radius (such as, NICER), or gravitational wave events (such as, LIGO and Virgo Collaborations) may help to break the degeneracy and constrain the other two quantities. Fortunately, Refs. [85, 86] recently reported the estimation of the radius and mass of PSR J0030+0451 based on the pulse-profile modeling of NICER data. The determination of the influence of newly reported constraints of mass and radius on the properties of neutron stars based on the parameterized EOS is in progress.

      We would like to thank Prof. Bao-An Li for constructive suggestions and comments.

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