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The research on the macroscopic properties of neutron stars is of great significance in revealing the internal composition and structure of neutron star. In this work, We analyze the influence of δmesons on the equation of states, the maximum mass, the tidal Love numbers and the tidal deformabilities for the conventional neutron stars and the hyperon stars within the relativistic mean field theory. It is found that the presence of δmesons can strengthen the tidal deformabilities of the low and medium-mass conventional neutron stars (or hyperon stars). However, the strengthening trends of the tidal deformabilities with δmesons gradually weaken with the increase of the mass of the conventional neutron stars (or hyperon stars). Especially for massive hyperon stars, the tidal deformabilities of the superstars with δmesons is weaker than the corresponding values without δmesons. Moreover, the presence of hyperons can reduce the tidal deformabilities of stars with the same mass. For the stars containing δmesons, only the tidal deformabilities in the hyperon stars with Λ, Σand Ξhyperons can satisfy the constraints of GW170817 and GW190814 events under the parameters selected in the paper. As the data about gravitational waves associated with the neutron stars gradually increase, there will be a possible way of judging the hyperon species in the hyperon stars.
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Keywords:
- neutron star/
- δmeson/
- tidal deformabilities
[1] [2] [3] [4] [5] [6] [7] [8] [9] [10] [11] [12] [13] [14] [15] [16] [17] [18] [19] [20] [21] [22] [23] [24] [25] [26] [27] [28] [29] [30] [31] [32] [33] [34] [35] [36] [37] [38] [39] [40] [41] [42] [43] [44] [45] [46] [47] [48] [49] [50] [51] [52] -
参数 $ {f}_{\sigma } $ $ {f}_{\omega } $ $ {f}_{\rho } $ $ {f}_{\delta } $ $ {g}_{2}/{\rm{f}\rm{m}}^{-1} $ $ {g}_{3} $ 不包含$ \rm{\delta } $介子 10.33 5.42 0.95 0.00 $ 0.033{g}_{\sigma }^{3} $ $ -0.0048{g}_{\sigma }^{4} $ 包含$ \rm{\delta } $介子 10.33 5.42 3.15 2.50 $ 0.033{g}_{\sigma }^{3} $ $ -0.0048{g}_{\sigma }^{4} $ 
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参数 $ {\rho }_{0}/{\rm{f}\rm{m}}^{-3} $ $ {E}_{\rm{s}\rm{y}\rm{m}}/\rm{M}\rm{e}\rm{V} $ $ L/\rm{M}\rm{e}\rm{V} $ $ {K}_{\rm{v}}/\rm{M}\rm{e}\rm{V} $ 不包含$ \rm{\delta } $介子 0.16 31.3 84 240 包含$ \rm{\delta } $介子 0.16 31.3 103 240 DownLoad:
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中子星最大质量处 中子星最大半径处 $ M/{\rm{M}}_{\odot } $ $ R/\rm{k}\rm{m} $ $ {k}_{2} $ Λtidal $ M/{\rm{M}}_{\odot } $ $ R/\rm{k}\rm{m} $ $ {k}_{2} $ Λtidal 1) 2.088 10.89 0.021 8 0.995 12.973 0.124 4405 2) 2.119 11.31 0.019 8 1.138 13.570 0.105 2417 3) 1.776 10.89 0.032 28 0.995 12.973 0.124 4405 4) 1.763 11.40 0.031 36 1.138 13.570 0.105 2417 5) 1.709 10.71 0.033 31 0.995 12.937 0.124 4405 6) 1.691 10.91 0.028 31 1.109 13.566 0.107 2791 DownLoad:
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R/km $ {K}_{2} $ $\varLambda$
($ 1.4{\rm{M}}_{\odot } $中子星)1) 12.80 0.090 545 2) 13.51 0.085 682 3) 12.81 0.090 548 4) 13.51 0.085 682 5) 12.58 0.084 468 6) 13.25 0.079 568 PSR J1903+0327
($ {1.666}_{-0.01}^{+0.01}{\rm{M}}_{\odot } $)1) [12.53, 12.56] [0.066, 0.067] [146, 162] 2) [13.26, 13.29] [0.061, 0.064] [180, 205] 3) [12.28, 12.37] [0.060, 0.063] [120, 140] 4) [13.04, 13.13] [0.058, 0.061] [158, 184] 5) [11.29, 11.48] [0.042, 0.046] [055, 070] 6) [11.49, 11.80] [0.034, 0.039] [050, 070] PSR J0453+1559
($ {1.559}_{-0.004}^{+0.004}{\rm{M}}_{\odot } $)1) [12.67, 12.68] [0.076, 0.077] [255, 265] 2) [13.39, 13.40] [0.072, 0.073] [313, 329] 3) [12.63, 12.64] [0.075, 0.075] [251, 256] 4) [13.37, 12.38] [0.071, 0.073] [309, 328] 5) [12.04, 12.08] [0.061, 0.062] [159, 169] 6) [12.61, 12.65] [0.055, 0.057] [179, 194] DownLoad:
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[1] [2] [3] [4] [5] [6] [7] [8] [9] [10] [11] [12] [13] [14] [15] [16] [17] [18] [19] [20] [21] [22] [23] [24] [25] [26] [27] [28] [29] [30] [31] [32] [33] [34] [35] [36] [37] [38] [39] [40] [41] [42] [43] [44] [45] [46] [47] [48] [49] [50] [51] [52]
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