Fig. 4.
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Correspondence of the observed QPOs to the overtones for the neutron star model with M = 1.6 M⊙ and 12 km. The QPOs observed in GRB 200415A can be identified with the first, second, fourth, and tenth overtones of crustal torsional oscillations, which leads to a suitable value of ς for the adopted stellar model of ς = 121.7 MeV.
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