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 3. The posterior distribution of Esym(2ρ0) constrained by assumed observed frequencies of 1.640 kHz, 1.720 kHz, and 1.800 kHz with a one percent relative error for a canonical neutron star (M = 1.4 M⊙). |
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