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

Kunjipurayil, Athul; Zhao, T.; Kumar, Bharat; Agrawal, Bijay K.; Prakash, Madappa

doi:10.1103/physrevd.106.063005

Cited by 34 publications

(12 citation statements)

References 104 publications

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“…This implies that the correlations of NS properties with individuals symmetry energy parameters are masked in the absence of appropriate constraints on the EoSs at low densities. It also partly explains why the outcome of the similar correlations studied in the earlier publications [31,34,36,39,45] are at variance. These correlations improve a little bit with the increase in the transition density.…”

Section: Discussionmentioning

confidence: 57%

“…The correlations of NS properties with various symmetry energy parameters and the pressure of β−equilibrated matter have been extensively investigated earlier using non-parametric [81], parametric [31,82], and physics-based models [34,36,38,39,81] and found to yield the results which are sometimes at variance, as summarized in Table III of Ref. [45]. Some of these studies include constraints imposed by bulk nuclear properties, while others have also imposed those through the constraints on nuclear matter parameters assuming them to be independent of each other.…”

Section: Neutron Star Properties and Symmetry Energy Parametersmentioning

confidence: 99%

“…Some of the factors that affect the correlations of NS properties with the nuclear matter parameters are also summarized in Table III of Ref. [45].…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Systematic analysis of the impacts of symmetry energy parameters on neutron star properties

Patra¹,

Venneti²,

Imam³

et al. 2023

Preprint

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Section: Discussionmentioning

confidence: 57%

Section: Neutron Star Properties and Symmetry Energy Parametersmentioning

confidence: 99%

See 1 more Smart Citation

Systematic analysis of the impacts of symmetry energy parameters on neutron star properties

Patra¹,

Venneti²,

Imam³

et al. 2023

Preprint

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“…A class of low frequency oscillations, known as f and g-modes, have received particular attention because their l = 2 multipolar component can couple with enough intensity to presently observed gravitational waves. Intensive work has been devoted to establish explicit relations between the frequency of different modes of pulsation and other properties of the star [43][44][45][46][47] or even with the EoS of the dense matter [45,[48][49][50][51][52][53][54][55][56].…”

Section: Introductionmentioning

confidence: 99%

Influence of hyperon–hyperon interaction on the properties of neutron stars

Aguirre

2024

J. Phys. G: Nucl. Part. Phys.

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The properties of neutron stars are studied in a composite modelof the strong interaction. In the regime of low to medium baryonicdensities a covariant hadronic model is adopted which includes anexclusive channel for the hyperon-hyperon interaction mediated byhidden strangeness mesons, which in turn couple to other mesonsthrough polynomial vertices. The new coupling constants aresubject to phenomenological constraints. The presence of freequarks in the core of the star is considered by using theNambu-Jona Lasinio model supplemented with a vector interaction.The deconfinement process is described by a continuous coexistenceof phases. Several structure parameters of neutron stars, such asmass-radius relation, moment of inertia, tidal deformability, andthe propagation of nonradial f and g-modes within the relativisticCowling approximation are studied. The predictions of the modelare in good agreement with recent observational data, inparticular the maximum inertial mass is greater than theobservational lower limit of two solar masses.

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“…The URs have been studied in subsequent works with different assumed NS EOS models or different NS compositions (Benhar et al 2004;Sotani et al 2011;Flores et al 2017;Ranea-Sandoval et al 2018;Das et al 2021;Jaiswal & Chatterjee 2021;Pradhan & Chatterjee 2021;Aguirre 2022;Pradhan et al 2022;Ranea-Sandoval et al 2022;Zhao & Lattimer 2022;Kumar et al 2023). Though initial URs involved the compactness (M/R) and mean density of the star, later works have shown that there exists universality of mode parameters with the inertia parameter (Lau et al 2010;Chirenti et al 2015), the tidal deformability parameters (Chen & Piekarewicz 2014;Pradhan et al 2023b), and with the nuclear parameters (Sotani 2021;Kunjipurayil et al 2022), which are helpful in different scenarios in the NS asteroseismology problem. Additionally, significant effort has been put forward to investigate the impact of rotation on the QNMs and the NS asteroseismology or URs (Kastaun et al 2010;Zink et al 2010;Gaertig & Kokkotas 2011;Yoshida 2012;Doneva et al 2013;Passamonti et al 2013;Pnigouras & Kokkotas 2016;Yazadjiev et al 2017;Rosofsky et al 2019;Krüger & Kokkotas 2020a, 2020b.…”

Section: Introductionmentioning

confidence: 99%

Constraining Nuclear Parameters Using Gravitational Waves from f-mode Oscillations in Neutron Stars

Pradhan,

Pathak,

Chatterjee

2023

ApJ

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Gravitational waves (GWs) emanating from unstable quasi-normal modes in neutron stars (NSs) could be accessible with the improved sensitivity of the current GW detectors or with the next-generation GW detectors and, therefore, can be employed to study the NS interior. Assuming f-mode excitation in isolated pulsars with typical energy of pulsar glitches and considering potential f-mode GW candidates for A+ (upgraded LIGO detectors operating at fifth observing run design sensitivity) and Einstein Telescope (ET), we demonstrate the inverse problem of NS asteroseismology within a Bayesian formalism to constrain the nuclear parameters and NS equation of state (EOS). We describe the NS interior within relativistic mean-field formalism. Taking the example of glitching pulsars, we find that for a single event in A+ and ET, among the nuclear parameters, the nucleon effective mass (m*) within 90% credible interval can be restricted within 10% and 5%, respectively. At the same time, the incompressibility (K) and the slope of the symmetry energy (L) are only loosely constrained. Considering multiple (10) events in A+ and ET, all the nuclear parameters are well constrained, especially m*, which can be constrained to 3% and 2% in A+ and ET, respectively. Uncertainty in the observables of a 1.4 M ⊙ NS such as radius ( R 1.4 M ⊙ ), f-mode frequency ( f 1.4 M ⊙ ), damping time ( τ 1.4 M ⊙ ), and a few EOS properties including squared speed of sound (c s 2) are also estimated.

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

Cited by 34 publications

References 104 publications

Systematic analysis of the impacts of symmetry energy parameters on neutron star properties

Systematic analysis of the impacts of symmetry energy parameters on neutron star properties

Influence of hyperon–hyperon interaction on the properties of neutron stars

Constraining Nuclear Parameters Using Gravitational Waves from f-mode Oscillations in Neutron Stars

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