Constraint on nuclear symmetry energy imposed by f-mode oscillation of neutron stars
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Constraint on nuclear symmetry energy imposed by f-mode oscillation of neutron stars |
| Jing Zhang,Dehua Wen,Yuxi Li |
| Figure 1. The prior distribution of f-mode frequencies of a neutron stars with known stellar masses and unknown stellar masses (assumed to be within 1.2–2.0 M⊙) under the simplified (set Esym(ρ0) = 31.7 MeV, L = 58.7 MeV, K0 = 240 MeV) parametric EOSs, which are already screened by the causality condition, the masses of observed massive neutron stars, and the tidal deformability of GW170817. |
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