g-mode Oscillations in Neutron Stars with Hyperons

Tran, V.H.; Ghosh, Suprovo; Lozano, Nicholas; Chatterjee, Debarati; Jaikumar, Prashanth

doi:10.48550/arxiv.2212.09875

Cited by 1 publication

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“…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. Notable QNMs include the fundamental mode (f -mode) [18][19][20], pressure mode (p-mode) [15,21], gravity mode (g-mode) [22][23][24][25][26][27][28][29], rotational mode (r-mode) [30][31][32][33][34][35], space-time mode (w-mode) [36,37], and other modes [38][39][40][41]. The frequencies of these oscillations are directly linked to the internal structure and composition of the stars [24].…”

Section: Introductionmentioning

confidence: 99%

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

Mohanty,

Ghosh,

Routaray

et al. 2024

J. Cosmol. Astropart. Phys.

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Anisotropy in pressure within a star emerges from exotic internal processes. In this study, we incorporate pressure anisotropy using the Quasi-Local model. Macroscopic properties, including mass (M), radius (R), compactness (C), dimensionless tidal deformability (Λ), the moment of inertia (I), and oscillation frequency (f), are explored for the anisotropic neutron star. Magnitudes of these properties are notably influenced by anisotropy degree. Universal I–f–C relations for anisotropic stars are explored in this study. The analysis encompasses various EOS types, spanning from relativistic to non-relativistic regimes. Results show the relation becomes robust for positive anisotropy, weakening with negative anisotropy. The distribution of f-mode across M–R parameter space as obtained with the help of C–f relation was analyzed for different anisotropic cases. Using tidal deformability data from GW170817 and GW190814 events, a theoretical limit for canonical f-mode frequency is established for isotropic and anisotropic neutron stars. For isotropic case, canonical f-mode frequency for GW170817 event is f 1.4 = 2.606+0.457 -0.484kHz; for GW190814 event, it is f 1.4 = 2.097+0.124 -0.149kHz. These relationships can serve as reliable tools for constraining nuclear matter EOS when relevant observables are measured.

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