Impacts of dark matter on the $f$-mode oscillation of hyperon star

Abstract

We investigate the f -mode oscillation of the dark matter admixed hyperon star within the relativistic Cowling approximation. The macroscopic properties are calculated with the relativistic mean-field (RMF) equation of states by assuming that the dark matter particles are inside it. The coupling constants between hyperons and scalar mesons are fixed by fitting with hyperon potential depth, while for hyperons and vector mesons, we use SU( 6) symmetry group method. The f -mode oscillation frequencies (only for l = 2) are calculated with four different neutron star equation of states. We also check the effects of hyperons/dark matter and hyperons with dark matter EOSs on the f -mode oscillations varying with different astrophysical quantities such as mass (M ), radius (R), compactness (M/R), surface red-shift (Zs), average density (ρ), dimensionless tidal deformability (Λ) of the neutron star. Some significant changes have been seen on the f -mode frequencies with and without hyperons/dark matter or hyperons+dark matter. Substantial correlations are observed between canonical frequency and Λ (f1.4 − Λ1.4) and maximum frequency and canonical Λ ( fmax − Λ1.4).

Probing the impact of delta-baryons on nuclear matter and non-radial oscillations in neutron stars

“…Within them, the fundamental f -mode holds special importance. In this section, we compute the f -mode frequency using Cowling approximation which deals with the condition that there will be no interaction between the motion of the fluids and metric perturbations [14][15][16]. Thus, the following differential equation may be used to determine the distinct oscillation modes of NS,…”

“…The exploration of these oscillation frequencies involves solving equations that describe fluid perturbations alongside equations that govern how matter and spacetime curvature interact in the presence of strong gravitational forces [12][13][14][15][16]. These oscillations are categorized into two primary types: radial and non-radial, both of which are subjects of active research.…”

The impact of anisotropy on neutron star properties: insights from 𝖨–𝖿–𝖢 universal relations

“…Neutron stars (NSs) exhibit oscillations that are regarded as potential sources of GWs, manifesting in various forms including radial [8][9][10][11][12][13] and non-radial [14][15][16][17] modes. When a NS experiences external or internal disturbances, it emits GWs through different oscillation modes known as quasi-normal modes (QNMs), each characterized by the restoring force that brings them back to their equilibrium state.…”