$f$-mode oscillations of compact stars in dynamical spacetimes: Equation of state dependencies and universal relations studies

Shashank, Swarnim; Nouri, Fatemeh Hossein; Gupta, Anshu

doi:10.48550/arxiv.2108.04643

Cited by 3 publications

(4 citation statements)

References 67 publications

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“…Hence the empirical relations from past works need to be modified. There are a few efforts to investigate the effect on f -modes of the inclusion of exotic forms of matter (hyperon or quark matter) [52,53,64,65,[76][77][78] or with current astrophysical constraints [79]. However, the works are either limited to selective EoSs or used Cowling approximation to find the mode characteristics.…”

Section: Inclusion Of Hyperonsmentioning

confidence: 99%

General relativistic treatment of $f$-mode oscillations of hyperonic stars

Pradhan,

Chatterjee,

Lanoye

et al. 2022

Preprint

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We present a systematic study of f -mode oscillations in neutron stars containing hyperons, extending recent results obtained within the Cowling approximation to linearized General Relativity. Employing a relativistic mean field model, we find that the Cowling approximation can overestimate the quadrupolar f -mode frequency of neutron stars by up to 30% compared to the frequency obtained in the linearized general relativistic formalism. Imposing current astrophysical constraints, we derive updated empirical relations for gravitational wave asteroseismology. The frequency and damping time of quadrupole f -mode oscillations of hyperonic stars are found to be in the range of 1.47 -2.45kHz and 0.13 -0.51 sec respectively. Our correlation studies demonstrate that among the various parameters of the nucleonic and hyperonic sectors of the model, the nucleon effective mass shows the strongest correlation with mode characteristics and neutron star observables. Estimates for the detectability of f -modes in a transient burst of gravitational waves from isolated hyperonic stars is also provided.

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Section: Inclusion Of Hyperonsmentioning

confidence: 99%

General relativistic treatment of $f$-mode oscillations of hyperonic stars

Pradhan,

Chatterjee,

Lanoye

et al. 2022

Preprint

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show abstract

“…However, the Cowling approximation gives reasonable results for the p 1 -mode with errors 15%. Unlike non-linear simulation of the f -mode oscillation which requires full GR [96,97], numerical simulation of the p 1 -mode could be simplified with the Cowling approximation, which is sufficiently accurate for most purposes.…”

Section: Discussionmentioning

confidence: 99%

“…Therefore, the error of the Cowling approximation in p 1 -mode 15%, which corresponds to p 1 -mode for stable NS with maximum mass. Given the fact that there's no 1% universal relation in the p-mode, the Cowling approximation can greatly simplify the equations especially in non-linear full GR simulations [96,97]. A 15% error from the Cowling approximation is acceptable for most purposes.…”

Section: F Accuracy Of the Cowling Approximationmentioning

confidence: 99%

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

Kunjipurayil¹,

Kumar²,

Agrawal³

et al. 2022

Preprint

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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.

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“…Hence, we provide the universal relations for Λ 3 and Λ 4 with Λ 2 for electric type, whereas for magnetic type, we provide the universal relation of Σ 2 and Σ 3 with Λ 2 . From the tidal deformability and mass obtained from a binary system, one can infer the NS radius (R) by using the EoS-independent relation that exists between stellar compactness (C = M/R), and tidal deformability parameter [39,43,47,[84][85][86] 2 . There are EoS-independent relations, which involve the tidal deformability of both binary NSs and binary parameters ( like q = m 1 /m 2 ).…”

Section: A Multipole Love and F-love Relationsmentioning

confidence: 99%

Impact of updated multipole Love numbers and f -Love universal relations in the context of binary neutron stars

2023

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Neutron star (NS) equation of state (EoS) insensitive relations or universal relations (UR) involving neutron star bulk properties play a crucial role in gravitational-wave astronomy. Considering a wide range of equations of state originating from (i) phenomenological relativistic mean field models, (ii) realistic EoS models based on different physical motivations, and (iii) polytropic EoSs described by spectral decomposition method, we update the EoS-insensitive relations involving NS tidal deformability (Multipole Love relation) and the UR between f-mode frequency and tidal deformability (f-Love relation). We analyze the binary neutron star (BNS) event GW170817 using the frequency domain TaylorF2 waveform model with updated universal relations and find that the additional contribution of the octupolar electric tidal parameter and quadrupolar magnetic tidal parameter or the change of multipole Love relation has no significant impact on the inferred NS properties. However, adding the f-mode dynamical phase lowers the 90% upper bound on Λ by 16-20% as well as lowers the upper bound of NSs radii by ∼500m. The combined URs (multipole Love and f-Love) developed in this work predict a higher median (also a higher 90% upper bound) for Λ by 6% and also predict higher radii for the binary components of GW170817 by 200-300m compared to the URs used previously in the literature. We further perform injection and recovery studies on simulated events with different EoSs in A+ detector configuration as well as with third generation (3G) Einstein telescope. In agreement with the literature, we find that neglecting f-mode dynamical tides can significantly bias the inferred NS properties, especially for low mass NSs. However, we also find that the impact of the URs is within statistical errors.

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$f$-mode oscillations of compact stars in dynamical spacetimes: Equation of state dependencies and universal relations studies

Cited by 3 publications

References 67 publications

General relativistic treatment of $f$-mode oscillations of hyperonic stars

General relativistic treatment of $f$-mode oscillations of hyperonic stars

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

Impact of updated multipole Love numbers and f -Love universal relations in the context of binary neutron stars

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