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It satisfies the following equation [132]: r4 j¯w′ ′ +4r 3 j′ ¯w=0,(29) wherej(r)≡e −[ν(r)+λ(r)]/2

First-order equations In this frame, ¯w(r)≡Ω−w 0(r)represents the angular velocity of the fluid element relative to the local inertial frame to orderΩ

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Quasiradial oscillations of rotating hybrid neutron stars

nucl-th · 2026-05-22 · unverdicted · novelty 4.0

Computes quasiradial frequencies of rotating neutron and hybrid stars in slow-rotation limit and identifies distinct spin-down behavior between the two classes using BHF, RMF, and Dyson-Schwinger EOS models.

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  • Quasiradial oscillations of rotating hybrid neutron stars nucl-th · 2026-05-22 · unverdicted · none · ref 2

    Computes quasiradial frequencies of rotating neutron and hybrid stars in slow-rotation limit and identifies distinct spin-down behavior between the two classes using BHF, RMF, and Dyson-Schwinger EOS models.