GW170817 implications on the frequency and damping time of fmode oscillations of neutron stars
Abstract
Within a minimum model for neutron stars consisting of nucleons, electrons and muons at equilibrium using about a dozen Equation of States (EOSs) from microscopic nuclear manybody theories and 40,000 EOSs randomly generated using an explicitly isospindependent parametric EOS model for highdensity neutronrich nucleonic matter within its currently known uncertainty range, we study correlations among the fmode frequency, its damping time and the tidal deformability as well as the compactness of neutron stars. Except for quark stars, both the fmode frequency and damping time of canonical neutron stars are found to scale with the tidal deformability independent of the EOSs used. Applying the constraint on the tidal deformability of canonical neutron stars extracted by the LIGO+VIRGO Collaborations from their improved analyses of the GW170817 event, the fmode frequency and its damping time of canonical neutron stars are limited to 1.67 kHz  2.18 kHz and 0.155 s  0.255 s, respectively, providing a useful guidance for the ongoing search for gravitational waves from the fmode oscillations of isolated neutron stars. Moreover, assuming either or both the fmode frequency and its damping time will be measured precisely in future observations with advanced gravitational wave detectors, we discuss how information about the mass and/or radius as well as the still rather elusive nuclear symmetry energies at suprasaturation densities may be extracted.
pacs:
97.60.Jd; 04.40.Dg; 04.30.w;95.30.SfI Introduction
If a neutron star is disturbed by an external or internal event, it may then oscillate nonradially and thus emit gravitational waves (GWs). The latter are generally expected to provide useful information about the structure and the underlying EOS of neutron stars. For a recent review on how/what information about the EOS of dense neutronrich matter can be extracted from studying the peak frequency of postmerger GW spectrum, frequencies of both quasiequilibrium and resonant tides in merging neutron star binaries as well as frequencies of various oscillating modes of isolated neutron stars, we refer the reader to ref. fcustipen (). Hopefully, the predicted features, see, e.g., those summarized in refs. Mot18 (); Blazquez2014 (), of GWs from quasinormal modes will be verified in the near future with advanced GW detectors, such as the Einstein Telescope Pitkin2011 (); sensitivities ().
The theoretical formalism for describing the GWs from the quasinormal oscillations of neutron stars has been well established, see, e.g., refs. Lindblom83 (); Detweiler85 (). The quasinormal modes can be classified into the polar and axial modes: the polar modes correspond to zonal compressions while the axial modes induce differential rotation in the fluid Andersson1996 (). In neutron stars, the polar modes can be coupled to fluid oscillations (the fundamental fmodes, pressure pmodes, and a branch of spacetime modes: the polar wmodes) while the axial modes are purely the spacetime modes of oscillations (the axial wmodes) Lau2010 (). Here we focus on the fmode as its relatively low frequency (1 3 kHz) makes it relatively easier to be observed than other modes Lau2010 (). For example, for a neutron star located at 10 kpc from us, Kokkotas et al. Kokkotas2001 () estimated that the energy required in the fmode in order to be detected with a signaltonoise ratio of 10 by the advanced LIGO detector is . It is far smaller than that for the pmode and wmode.
There are several different ways to stimulate the pulsation modes Kokkotas2001 (): (a) A supernova explosion. An optimistic estimate for the energy radiated as the GW from supernovae can be up to about M. (b) A starquake associated with a pulsar glitch. The typical energy released in this process is estimated to be about Mock1998 (). (c) A binary neutron star merger remnant. Before the remnant collapses to a black hole, it is expected that several oscillation modes can be excited Baumgarte1996 (). Moreover, the oscillation modes of individual neutron stars can also be excited by the tidal fields before they merger Kokkotas1995 (). (d) A prominent phase transition, which can lead to a minicollapse in neutron stars and thus results in a sudden softening of the EOS. An optimistic estimate for the energy radiated as GWs could be up to MKokkotas2001 (); Lin2011 ().
While the above expectations/estimates are based on solid theoretical studies, essentially none of them have been observationally confirmed yet. Thus, relating them with existing observations is very useful. The first detection of a binary neutron star merger event GW170817 has opened a new window for understanding properties and the EOS of neutron stars. Indeed, many interesting physics, see, e.g., refs. Margalit2017 (); Rezzolla2018 (); Ruiz2018 (); LIGO2018 (); Annala2018 (); Most2018 (); De2018 (), has been extracted from the historical event GW170817. One key quantity extracted from the GW170817 is the tidal deformation LIGO2018 () for canonical neutron stars of mass 1.4M. It would thus be interesting to investigate if/how the extracted tidal deformability may help constrain any features of the fmode oscillations of neutron stars. We find that the fmode frequency and damping time for canonical neutron star are limited to 1.67 kHz  2.18 kHz and 0.155 s  0.255 s, respectively. As refined measurements of the tidal deformability for more merger events are expected, tighter constraints on the fmode will come. In turn, future measurements of the fmode frequency and damping time themselves will help crosscheck results from other approaches in the era of multimessenger astronomy.
It is easy to understand that the GWs emitted from the quasinormal modes carry useful information about global properties and the internal structure as well as the EOS of neutron stars. But how can we decipher this information from the detected GWs? Normally, one investigates features, such as the frequency and damping time, of quasinormal modes through numerically solving differential equations governing the perturbed metric with model EOSs of neutron star matter. If we called this route as the “direct” way that is basically straightforward given an EOS, the “inverse” approach (i.e., using the observed fmode features to infer properties and the underlying EOS of neutron stars) is not easy because the related differential equations is too complicated to be numerically inverted. Besides the standard Bayesian inference, a practically useful way is to make use of the well established universal relations (independent of the EOS of neutron star matter) revealed in studying the frequency and damping time of the quasinormal modes and their dependences on the compactness of neutron stars, see, e.g., refs. Blazquez2014 (); Andersson1996 (); Lau2010 (). Obviously, if the universal relations are correct, one can use observed GW features to determine the scaling parameters, such as the stellar mass, radius and moment of inertia. Can we further determine the underlying EOS? The answer is yes since the global properties depend strongly on the EOS. We shall explore if/how this may be done after verifying some of the well known universal relations.
The paper is organized as follows. In Sec. II, the parametric EOS of dense neutronrich nucleonic matter is outlined. In Sec. III, we first recall the differential equation governing the complex frequency of the fmode. We then study the correlations between the fmode frequency (damping time) and the tidal deformation. Constraints on the fmode frequency and its damping time by the tidal deformation of canonical neutron stars extracted from the GW170817 event are then presented. In Sec. IV, a brief review on the universal relations of the fmode oscillations is given. In Sec. V, we discuss how information about global properties of neutron stars and the highdensity behavior of nuclear symmetry energy can be extracted assuming either or both the fmode frequency and damping time are measured accurately. A summary of the main points is given at the end.
Ii An explicitly isospindependent EOS for dense neutronrich nucleonic matter
For ease of our following discussions, we briefly outline here how we construct the EOS within a minimum model for neutron stars consisting of neutrons, protons, electrons and muons at equilibrium. More details can be found in ref. Zhang2018 (). We use the NV EOS Negele73 () for the inner crust and the BPS EOS Baym71 () for the outer crust. The transition point to the liquid core is found by studying where/when the incompressibility of uniform neutron star matter becomes imaginary, see detailed discussions in ref. Zhang2018 (). For the EOS of the core, there are many predictions based on various nuclear manybody theories using different interactions. The predicted EOSs from different theories often diverge especially at suprasaturation densities. Thus, to minimize model dependence in preparing the EOS of neutron star matter while be flexible and inclusive enough to cover all EOSs allowed by all known constraints, here we adopt the rather general parametric EOS model for neutronrich nucleonic matter in the core Zhang2018 (). The total pressure as a function of energy density for the charge neutral matter at equilibrium is calculated selfconsistently. As a basic input, the nucleon specific energy of neutronrich matter with isospin asymmetry can be well approximated by the empirical parabolic law as Bombaci1991 (); Li2008 ():
(1) 
where and are the energy in symmetric nuclear matter and the symmetry energy of asymmetric nuclear matter, respectively. They can be conveniently parameterized as
(2) 
(3)  
According to the existing knowledge on the parameters near the saturation density of nuclear matter, the most probable values of them are as follows: MeV, MeV, MeV, and MeV, MeV, MeV, see, e.g., refs. Shlomo06 (); Piekarewicz10 (); Li13 (); Zhang17 (); Oertel17 (); Li17 (). The first three parameters , and have already been constrained in a narrow range, while the last three parameters , and still have very large uncertainties. It is worth emphasizing that the above expressions have the following dual meanings: they are Taylor expansions near the saturation density for systems with low isospin asymmetries. For very neutronrich systems especially at suprasaturation densities, they are simply parameterizations. Thus, the highdensity parameters , and are no longer Taylor expansion coefficients, but free parameters to be determined by observations of neutron stars and/or highenergy heavyion reaction experiments especially with radioactive beams Zhang2018 (). However, the uncertainty ranges of these parameters cited above mostly based on nuclear theory predictions provide a useful reference (the ranges of prior probability distribution functions of these parameters in Bayesian analyses) for their eventual inference from the experimental/observational data. By varying the EOS parameters, we can generate efficiently large numbers of EOSs for neutron star matter. These EOSs are first screened against the well accepted constraints, such as, the causality condition and the ability to support neutron stars with masses at least as high as 2.01 M, etc.
For comparisons, we also use 11 EOSs from predictions of microscopic nuclear manybody theories for normal or hybrid neutron stars (marked as 11 microscopic EOSs in the following text and figures) and 2 EOSs from the MIT bag model for quark stars. The 11 microscopic EOSs include: ALF2 of Alford et al. ALF2 () for hybrid (nuclear + quark matter) stars, APR3 and APR4 of Akmal and Pandharipande AP34 (), ENG of Engvik et al. ENG (), MPA1 of Muther, Prakash and Ainsworth MPA1 (), SLy of Douchin and Haensel SLy (), WWF1 and WWF2 of Wiringa, Fiks and Fabrocini WFF12 (), the QMFL40, QMFL60 and QMFL80 within the Quark Mean Field model with L=40, 60 and 80 MeV, respectively, from the recent work of Zhu et al. QMF (). The two EOSs of quark stars are from the MIT bag model with the pressure as a function of energy density given by with the bag constant B=30 and 57 , respectively Chodos1974 (); Glendenning1997 ().
Iii Constraints on the fmode frequency and damping time by the tidal deformation of neutron stars
According to the work of Lindblom and Detweiler, the perturbed metric of nonradial oscillating neutron stars can be written as Lindblom83 (); Detweiler85 ()
(4)  
The fluid element of perturbation can be expressed by the Lagrangian displacement components as
(5) 
(6) 
(7) 
where the , , , and are perturbation functions, and the is the spherical harmonic function. They are not all independent. The perturbed metric function can be represented by other two perturbed functions as Lindblom83 (); Detweiler85 ()
(8)  
By using linearized Einstein equations and the continuity equation, a set of fourthorder differential equations can be deduced as the following Lindblom83 (); Detweiler85 ()
(9)  
(10)  
(11)  
(12)  
where the prime represents the firstorder derivative with respect to radius, such as , the quantity is the adiabatic index, and the function (to replace ) is defined as
(13) 
To numerically solve the perturbation equations, one can integrate the Eqs. (9)(12) from the center to the surface of neutron stars. The initial values at the center are taken as
(14)  
(15)  
(16) 
The unique solution with a specific complex frequency is determined by the condition at the stellar surface Kokkotas1999 (). The fmode oscillation frequency and its damping time are determined by the real and imaginary parts of , respectively. For detailed discussions of the numerical method to solve the above equations, we refer the reader to refs. Lindblom83 (); Detweiler85 (); Benhar04 (); Miniutti03 (). The code we used to calculate the fmode frequency and damping time is the same one we used earlier in ref. Wlin14 ().
Among the properties of neutron stars extracted from analyzing the GW170817 event, the tidal deformation is the most important one carrying information about the EOS of neutron star matter. The dimensionless tidal deformability is defined using the second Love number , stellar mass and radius as
(17) 
The depends on not only the mass and radius but also the interior structure of neutron stars. Numerically, it is determined through a very complicated differential equation Hinderer2010 () coupled to the TolmanOppenheimerVolkov (TOV) equation TOV () for a given EOS. The code we used to calculate the is the same one used previously in refs. Fattoyev2013 (); Fattoyev2014 ().
Within the parametric EOS mode outlined in Sect. II, we generated 40,000 EOSs for neutron stars in the following way: the parameters characterizing the EOS near the saturation density of nuclear matter are fixed at their most probable values known, i.e., MeV, MeV and MeV; while the parameters describing the highdensity behavior of nuclear EOS are randomly selected with equal probabilities in the ranges of MeV, MeV and MeV, respectively. After removing those (1) violating the causality condition, or (2) can not support the currently observed most massive neutron star of mass Antoniadis13 (), (3) or leading to mechanical instabilities at any density, over 23,000 rational EOSs are left for further studies.
We now explore possible correlations between the fmode characteristics and the tidal deformability of neutron stars. Such correlations may exist because it has been well known that both the fmode frequency and its damping time scale with the compactness M/R independent of the EOS, see, e.g., refs. Andersson1996 (); Tsui2005b (), while the tidal deformability has also been found to depend strongly on the although the is still rather EOS model dependent Zhang2019 (). Our results for a fixed stellar mass of are presented in Figs. 1 and 2. It is very interesting to see that an almost perfect universal correlation exists between the frequency/damping time and the tidal deformability except for the two quark EOSs. It is not surprising that the and versus relations with the quark star EOSs do not fall onto the same universal relations as with the other EOSs used. Indeed, both the (or versus M/R and versus M/R universal relations were suggested earlier without considering any quark star model Tsui2005b (); Yagi2013 (). One possible reason is that both the tidal deformability and the fmode characteristics ( and ) depend strongly on the internal structure of neutron stars. Indeed, the structure of quark stars is quite different from the normal ( matter with or without hyperons) neutron stars which have a characteristic lowdensity crust. As a result, their massradius relations are very different, leading to the distinct and versus relations.
The universal and versus relations may have some significant applications. Obviously, they enable us to constrain the predicted features of fmode oscillations using the existing data on the tidal deformability of neutron stars and terrestrial laboratory constrains on the EOS parameters. It is seen that for a fixed stellar mass of , the lowest tidal deformability allowed by the parametric EOS is 165, which is higher than the lower limit of extracted from analyzing the GW170817 event LIGO2018 (). While the revised maximum tidal deformability from the improved analyses LIGO2018 () of the GW170817 event limits both the fmode frequency and damping time. Therefore, by combining the two constraints: the EOS parameter space allowed by existing terrestrial nuclear laboratory experiments and the tidal deformation extracted from GW170817, the fmode frequency and damping time for a neutron star are constrained in the region of 1.67 kHz  2.18 kHz and 0.155 s  0.255 s, respectively, providing a useful guidance for detecting GWs from fmode oscillations of neutron stars. As more neutron star mergers are expected to be measured more accurately, the further reduced uncertainty of the tidal deformability especially about its lower limit will constrain more tightly the fmode features. Moreover, the and versus relations of quark stars deviate distinctly from those universal relations of normal neutron stars, providing a possible way of distinguishing the two kinds of neutron stars.
To this end, it is very interesting to mention that simulations of merging neutron star binaries have found that the mass scaled frequency (peak frequency) at the maximum amplitude on the spectrum of the postmerger GWs scales approximately universally with some powers of the tidal deformability or compactness independent of the EOSs used Bau12 (); Rea13 (); Ber1 (); Ber2 (). If the remnant formed after the merger can be instantaneously approximated by a perturbed differentially rotating star, the fmode of pulsation is strongly excited and it is the most efficient channel for GW emissions Ber2 (). Thus, the scaling of the peak frequency in the binary mergers can be related to the fmode frequency of isolated neutron stars. Indeed, Nils Andersson pointed out that the correlation between the peak frequency and the tidal deformability in neutron star mergers is in principle “expected” from results of the oscillating single neutron stars fcustipen (). Clearly, our results presented above support his expectation. The common feature shared by the peak frequency in postmerger spectrum and the fmode frequency of isolated neutron stars indicate that the differential rotations and thermal effects do not significantly affect the oscillations.
Iv Scalings of the fmode frequency and damping time with the compactness of neutron stars of fixed masses
We first recall here what have been known in the literature about some universal scalings of the fmode frequency and damping time with respect to the compactness and its variations of neutron stars. We then compare our results from using the 23,000 parametric EOSs with the well established scalings. To our best knowledge, since the early work of Andersson and Kokkotas Andersson1996 (); Andersson1998 (), many groups have investigated the universality in characteristics of quasinormal modes of neutron stars, see, e.g., refs. Benhar2004 (); Tsui2005 (); Wen2009 (); Lau2010 (); Blazquez2013 (); Blazquez2014 (); Chirenti2015 (); Stergioulas2018 (). It is worth noting that all the universal relations reported are not absolutely independent of the EOSs and we focus on the fmode in this study.
The first widely cited equations to describe the universal relation of fmode come from the work of Andersson and Kokkotas Andersson1998 (). They found that the fmode frequency and damping time can be parameterized respectively as
(18) 
(19) 
where , and are model independent constants. These universal relations have the features that the frequency of the fmode is proportional to the square root of the stellar average density, while the scaled damping time is a function of the compactness . We note that quark stars are not considered in obtaining the above relations. Two other interesting universal relations were given in refs. Tsui2005b (); Lau2010 (). In particular, the following parameterization can be used for most of the quasinormal modes (the polar fmode, 1st polar wmode, 2nd polar wmode, 1st axial wmode and the 2nd axial wmode) Tsui2005b ()
(20) 
where , and are complex constants and have individual values for each mode. For the fmode, , , and . It is obvious that the complex eigenfrequency only depends on the compactness . This universal relation also does not include quark stars. The following is their other universal relation given in terms of the effective compactness, , where I is the moment of inertia Lau2010 ()
(21) 
(22) 
This universal relation works well for both normal neutron stars and quark stars, and have a better accuracy than earlier universal relations. They argue that the effective compactness is a better quantity to characterize the internal mass profile of neutron stars.
BlazquezSalcedo et al. obtained the following universal relation directly relating the frequency (scaled by the radius) and the damping time (scaled by the mass) Blazquez2014 ()
Again, quark stars are not considered in deriving this relation.
More recently, Stergioulas et al. Stergioulas2018 () extended the universal relation for the damping time of fmode to higher orders and compared it with that in refs. Andersson1998 (); Tsui2005b (). It reads
(24) 
This universal relation has a higher accuracy (with a standard statistical correlation coefficient 0.9997) in a wide range of compactness ().
To this end, it is necessary to compare our results with the well established universal relations mentioned above. Indeed, we found general agreements with the existing relations. As an example, we compare in Fig. 3 our results using the 23,000 parameterized EOSs with the universal relation of Eq. (20) given in ref. Tsui2005b () for a fixed stellar mass of 1.4 M. The TVIIM (red line) result was obtained from using a simple TVIIM model (the Tolman VII model Tolman1939 ()) to approximate the mass profile inside neutron stars, while the realistic stars (blue dashed line) was obtained by fitting the EOSs predicted by eight different models (APR1,APR2, AU, GM24, MODEL A, MODEL C, UT and UU), for details about these EOS models we refer the reader to refs. Tsui2005b (). It is seen that our results obtained by using the parameterized EOSs are generally consistent with the universal relation of Eq. (20) using the two different sets of EOSs. As we mentioned earlier and shown in Fig. 3, the scalings between the frequency and compactness or the average density are not absolutely EOSindependent especially for neutron stars with very low or high compactness. However, as we shall discuss next and shown in Figs. 46, there is a perfect universal relation between the fmode frequency and its damping time for neutron stars with fixed masses using all EOSs including those for quark stars.
V Applications of the universal relation between the frequency and damping time of fmode oscillations of neutron stars with fixed masses
According to the estimates of Kokkotas et al., the relative error in extracting the fmode frequency can be up to assuming a signaltonoise ratio of 10 Kokkotas2001 (). Thus, the frequency can be measured rather accurately. If both the frequency and/or damping time of the GW emitted from the fmode oscillation of a neutron star can be accurately measured in the near future, what can we learn about the global properties of neutron stars and the underlying EOS of dense neutronrich nuclear matter? Here we try to answer this question at least partially to the best we can. In principle, using the parametric EOS one can solve the inversestructure problem of neutron stars as demonstrated recently in refs. Zhang2018 (); Zhang2019b () to find all necessary combinations of the EOS parameters to produce a given observable or use techniques of Bayesian analyses to infer the probability distribution functions of all EOS parameters from the observational data. As an alternative, here we explore the possibility of inferring global properties of neutron stars and the underlying EOS using the universal relations between the fmode frequency and its damping time of neutron stars with fixed masses assuming both of them can be obtained accurately from observations.
Using the same sets of EOSs as in Sec. II, the correlation between the fmode frequency and its damping time for a canonical neutron star is shown in Fig. 4. It is seen that both the normal neutron stars and quark stars for a given mass fall onto the same universal relation independent of the EOSs used. This finding is not surprising. As outlined in Sect. III, the differential equations governing the fmode complex frequency as a whole depend on the EOS through the pressure . Since the real and imaginary parts of the complex frequency vary coherently with the EOS, their dispersion relation for neutron stars with the same mass fall onto the same curve. This is very different from inspecting individually the frequency and damping time as functions of the compactness or tidal deformability which by itself varies with the EOS. To further illustrate this point, the universal relations with different stellar masses are shown in Figs. 5 and 6. As expected, from light to massive neutron stars, the perfect universality between the fmode frequency and its damping time always holds. Thus, if both the frequency and/or damping time of the GW emitted from the fmode oscillation of a neutron star can be accurately measured, some global properties of neutron stars can be extracted. For example, if a frequency of kHz is observed from a neutron star of known mass 1.4 M, then the damping time should be 0.218 s  0.223 s from inspecting the correlations shown in Fig. 5, and the stellar radius should be 12.23 km 12.69 km from inspecting the correlation shown in Figs. 3 and 5. Properties corresponding to another example with a measured frequency of kHz are given also in Fig. 5.
Using the results shown in Fig. 6 we illustrate what we can learn if both the fmode frequency and its damping time can be measured but from an isolated neutron star of an unknown mass. Shown are the universal relations for three neutron stars with similar masses of M M and M, respectively. The three relations are clearly separated. If both the frequency and damping time can be obtained simultaneously with some precisions from future observations, such as, kHz and =0.22 s, then the stellar mass should be around M.
One of the major goals of studying properties of neutron stars is to understand and constrain the underlying EOS of dense neutronrich nuclear matter. While the isospin symmetric part of the EOS has been relatively tightly constrained by terrestrial nuclear laboratory experiments Pawel (), the density dependence of nuclear symmetry energy has been the most uncertain part of the EOS of dense neutronrich nucleonic matter TEsym (). While significant progress has been made in probing the using nuclear experiments, the highdensity behavior of remains rather elusive Li17 (); TEsym (). We now explore to what extent the GWs from fmode oscillations may help constrain the highdensity behavior of nuclear symmetry energy. As examples, we assume that two possible frequencies (1.640 kHz and 1.800 kHz) are detected with a 1% accuracy for a neutron star of mass 1.4 M, then only some values of the highdensity symmetry energy parameters and are allowed, leading to a constraint on the at suprasaturation densities. Our results are shown in Figs. 7 and 8 for the frequency of 1.640 kHz and 1.800 kHz, respectively. In both cases, the spreads further out as the density increases. Since the symmetry energy around twice the saturation density is especially important for determining the radii of neutron stars Lattimer01 (), it is useful to compare specifically the constraints on the . If a lower (higher) frequency of 1.640 kHz (1.800 kHz) is observed, then a higher (lower) value of MeV ( MeV) can be inferred. Comparing the results in Figs. 7 and 8, it is seen that a variation of about 9% in frequency leads to about 22% change in the value of extracted. Moreover, the tendency of the symmetry energy at even higher densities are also quite different. To put the numerical results in perspective, we note that an extrapolation of the experimental systematics from subsaturation to suprasaturation densities predicted that LWC15 (). A recent study of neutron star radii and tidal deformability indicated that MeV Zhang2019b (), while predictions based on nuclear manybody theories scatter between and 100 MeV Zhang2019b (). Compared to these earlier results especially the rather diverge theoretical predictions, obtaining the limits on the from the supposed detection of the fmode frequency with a 1% accuracy would be a significant progress in the field of highdensity nuclear EOS studies.
Vi Summary
In summary, within a minimum model for neutron stars using 11 EOSs from microscopic nuclear manybody theories, 2 EOSs from the MIT bag model for quark stars and 40,000 parametric EOSs with their parameters constrained by all existing constraints mostly from terrestrial nuclear laboratory experiments, we studied the correlations among the fmode frequency and its damping time as well as the tidal deformability and compactness of neutron stars. Besides verifying some of the well established universal relations in the literature, we find that

Except for quark stars, both the fmode frequency and its damping time scale with the tidal deformability of canonical neutron stars independent of the EOSs used.

The tidal deformability from analyzing the GW170817 event limits the fmode frequency and damping time of canonical neutron stars to 1.67 kHz  2.18 kHz and 0.155 s  0.255 s, respectively, providing a useful guidance for the ongoing search for gravitational waves from the fmode oscillations of neutron stars.

The fmode frequency and its damping time strongly correlate with each other for neutron stars of the same masses. If both of them can be obtained with high accuracies from future observations, their correlations allow for the accurate extraction of neutron star global properties and knowledge about the EOS of dense neutronrich nuclear matter. Several numerical examples under idealized conditions were considered. In particular, nuclear symmetry energy at twice the saturation density can be extracted with an accuracy compatible with that of several other approaches available.
Indeed, gravitational waves from the fmode oscillations of neutron stars provide useful and complimentary information about both properties of neutron stars and the underlying EOS of dense neutronrich nuclear matter.
Acknowledgements.
We would like to thank WenJie Xie for helpful discussions. This work was supported in part by the U.S. Department of Energy, Office of Science, under Award Number DESC0013702, the CUSTIPEN (ChinaU.S. Theory Institute for Physics with Exotic Nuclei) under the US Department of Energy Grant No. DESC0009971 and the National Natural Science Foundation of China under Grant Nos. 11275073, 11320101004, 11675226 and 11722546.References
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