Universal Relations for Neutron Star F-Mode and G-Mode Oscillations

Lattimer, James M

doi:10.48550/arxiv.2204.03037

Cited by 9 publications

(19 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The f -mode of neutron stars correlates with many NS properties including compactness [19], moment of inertia [20] and static tidal polarizability [21,22]. Such universal relations hold even for bare quark stars without crust or hybrid NSs with first order transitions [3]. However, p-modes have very weak correlation with other NS properties [19].…”

Section: Introductionmentioning

confidence: 95%

“…Many previous studies have used the Cowling approximation [27][28][29][30], which lacks dissipation due to gravitational waves. The Cowling approximation introduces about a 20-30% error in the f -mode frequency [3,[31][32][33], which is significantly less accurate than that of the Ω f − Ī − Λ universal relations. A 10% error in the compositional g-mode frequency [2] and 19% error in the discontinuity g-mode frequency [3,32] from the Cowling approximation has also been found.…”

Section: Introductionmentioning

confidence: 97%

“…The Cowling approximation introduces about a 20-30% error in the f -mode frequency [3,[31][32][33], which is significantly less accurate than that of the Ω f − Ī − Λ universal relations. A 10% error in the compositional g-mode frequency [2] and 19% error in the discontinuity g-mode frequency [3,32] from the Cowling approximation has also been found. However, the accuracy of the Cowling approximation for the and p-mode is not well quantified.…”

Section: Introductionmentioning

confidence: 97%

“…Moreover, these modes mainly contribute to a NS's gravitational wave emission. In order to study these oscillation frequencies, we need to solve the fluid perturbation equations along with the Tolman-Oppenheimer-Volkoff (TOV) equations in general relativity (GR) [2,3].…”

Section: Introductionmentioning

confidence: 99%

“…The peak frequency in supermassive NSs is almost equal to that of the non-rotating f -mode frequency of isolated NSs with the same mass as each of the merging components [10]. With third generation gravitational wave telescopes such as the Cosmic Explorer [11] and Einstein telescope [12], the predicted event rate improves further to 0.06 yr −1 to 4 yr −1 , which is promising [3,13].…”

Section: Introductionmentioning

confidence: 99%

See 4 more Smart Citations

Impact of the equation of state on $f$- and $p$- mode oscillations of neutron stars

Kunjipurayil¹,

Kumar²,

Agrawal³

et al. 2022

Preprint

Self Cite

View full text Add to dashboard Cite

We investigate the impact of the neutron-star matter equation of state on the f -and p1-mode oscillations of neutron stars obtained within the Cowling approximation and linearized General relativity. The f -and p1-mode oscillation frequencies, and their damping times are calculated using representative sets of Skyrme Hartree-Fock and relativistic mean-field models, all of which reproduce nuclear systematics and support 2M neutron stars. Our study shows strong correlations between the frequencies of f -and p1-modes and their damping times with the pressure of β-equilibrated matter at densities equal to or slightly higher than the nuclear saturation density ρ0. Such correlations are found to be almost independent of the composition of the stars. The frequency of the p1-mode of 1.4M star is strongly correlated with the slope of the symmetry energy L0 and β-equilibrated pressure at density ρ0. Compared to GR calculations, the error in the Cowling approximation for the f -mode is about 30% for neutron stars of low mass, whereas it decreases with increasing mass. The accuracy of the p1-mode is better than 15% for neutron stars of maximum mass, and improves for lower masses and higher number of radial nodes.

show abstract

Section: Introductionmentioning

confidence: 95%

Section: Introductionmentioning

confidence: 97%

Section: Introductionmentioning

confidence: 97%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

Impact of the equation of state on $f$- and $p$- mode oscillations of neutron stars

Kunjipurayil¹,

Kumar²,

Agrawal³

et al. 2022

Preprint

Self Cite

View full text Add to dashboard Cite

show abstract

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.

View full text Add to dashboard Cite

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.

show abstract

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

Kalita,

Routaray,

Ghosh

et al. 2024

J. Cosmol. Astropart. Phys.

View full text Add to dashboard Cite

Non-radial oscillations of Neutron Stars (NSs) provide a means to learn important details regarding their interior composition and equation of state. We consider the effects of Δ-baryons on non-radial f-mode oscillations and other NS properties within the Density-Dependent Relativistic Mean Field formalism. Calculations are performed for Δ-admixed NS matter with and without hyperons. Our study of the non-radial f-mode oscillations revealed a distinct increase in frequency due to the addition of the Δ-baryons with upto 20% increase in frequency being seen for canonical NSs. Other bulk properties of NSs, including mass, radii, and dimensionless tidal deformability (Λ) were also affected by these additional baryons. Comparing our results with available observational data from pulsars (NICER) and gravitational waves (LIGO-VIRGO collaboration), we found strong agreement, particularly concerning Λ.

show abstract

Universal Relations for Neutron Star F-Mode and G-Mode Oscillations

Cited by 9 publications

References 0 publications

Impact of the equation of state on $f$- and $p$- mode oscillations of neutron stars

Impact of the equation of state on $f$- and $p$- mode oscillations of neutron stars

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

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

Contact Info

Product

Resources

About