The gravitational wave $\omega$ mode spectrum presents a unique window into the dense interior of neutron stars, probing physics inaccessible to electromagnetic observations. This work investigates the $\omega$ modes of compact stars composed of quarkyonic matter. The quarkyonic model, which describes a crossover transition between nucleonic and quark matter treated as quasiparticles, is formulated within the relativistic mean-field (RMF) theory using the G3 and IOPB-I parametrizations. This core is surrounded by a mantle of hadronic matter, creating a multicomponent stellar interior. The overall equation of state (EOS) is governed by two key parameters: the transition density ($n_t$), and the QCD confinement scale (${\mathrm{\Lambda }}_{\mathrm{cs}}$), which are varied to construct models consistent with current astrophysical constraints on mass and radius. We compute the complex eigenfrequencies (damped oscillations) of the fundamental and first excited $\omega$ modes using the phase-amplitude method within a full general relativistic framework. Our simulations reveal that the admixed quarkyonic structure produces a unique $\omega$ mode signature, distinctly different from pure hadronic or hybrid stars. The spectrum exhibits a strong, degenerate dependence on the EOS, where the stiffening effect of the quarkyonic matter influences oscillation frequencies and damping times in a characteristic manner. We also demonstrate that $\omega$ mode frequencies for quarkyonic stars follow approximate universal relations, largely independent of the EOS.

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• Neutron stars & pulsars