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 6. Different constraints on the symmetry energy Esym(ρ). (a) The black area represents the prior constraint for which no screening conditions are imposed on the EOSs. (b) The red area represents the prior constraint for which the EOSs are screened by the abovementioned three conditions. (c) The green area represents the posterior constraint (with a 90% credibility interval) for an assumed observed frequency if 1.720 kHz (with 1% of relative error). (d) The blue area represents a posterior constraint similar to (c) but for a canonical neutron star with a 1.720 kHz f-mode frequency. |
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