Effect of hyperons on 
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-mode oscillations in neutron stars

Pradhan, Bikram Keshari; Chatterjee, Debarati

doi:10.1103/physrevc.103.035810

Cited by 38 publications

(37 citation statements)

References 52 publications

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“…We tabulated the value of f max and f 1.4 for four different RMF forces with different NS observables in Table III. The mass variation of frequency changes within interval 1.75-2.55 kHz for l = 2, which is almost consistent with Pradhan et al [63] for the considered parameter sets. For hyperons/DM3 and hyper-ons+DM3 cases, the frequency range within interval 1.8-2.85 kHz is higher than the earlier case.…”

Section: A Calculation Of F -Mode Frequency As Functions Of Different...supporting

confidence: 91%

“…Hence, it emits gravitational waves with different modes of frequencies. The most important modes are fundamental mode (f ), first and second pressure modes (p), and the first gravitational mode (g) [16,21,63]. Almost all the energy of the NS are emitted as GWs radiations with these modes.…”

Section: Calculation Of F -Mode Oscillation Of the Nsmentioning

confidence: 99%

“…In this, work we want to calculate the non-radial oscillations of the NS using the Cowling approximations for a DM admixed hyperon star. To find different oscillations mode frequencies, one has to solve the following coupled differential equations [19][20][21]63] dW (r)…”

Section: Calculation Of F -Mode Oscillation Of the Nsmentioning

confidence: 99%

“…IV In this section, we adopt the RMF model to calculate the NS properties. In RMF model, the nucleons interact with each other by exchanging different mesons such as isoscalar-scalar (σ), isoscalar-vector (ω), isovector-vector (ρ), isovector-scalar (δ) [58][59][60][61] and the hyperon-hyperon interaction is mediated by the two additional strange mesons, strange scalar (σ * ) and strange vector (φ) [46,62,63]. Hence, the Lagrangian of the system includes the interaction from mesons-nucleons, mesons-hyperons and their self and cross-couplings.…”

Section: Introductionmentioning

confidence: 99%

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

Das,

Kumar,

Biswal

et al. 2021

Preprint

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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).

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Section: A Calculation Of F -Mode Frequency As Functions Of Different...supporting

confidence: 91%

Section: Calculation Of F -Mode Oscillation Of the Nsmentioning

confidence: 99%

Section: Calculation Of F -Mode Oscillation Of the Nsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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

Das,

Kumar,

Biswal

et al. 2021

Preprint

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“…In this context, it has been suggested that the study of the non-radial oscillation modes of neutron stars can have the possibility of providing the compositional information regarding the matter in the interior of the neutron stars. This includes the neutron stars with a hyperon core [40][41][42], a quark core or a mixed phase with quark and hadronic matter components [39,[43][44][45][46][47][48]. This is because the non-radial oscillations not only depend upon the EOS i.e.…”

Section: Introductionmentioning

confidence: 99%

Non-radial oscillation modes in hybrid stars: consequences of a mixed phase

Kumar¹,

Mishra²,

Malik³

2021

Preprint

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We study the possible existence of deconfine quark matter in the core of neutron stars. A relativistic mean field model is used to describe the nuclear matter at low densities while Nambu-Jona-Lasinio model is used to describe the quark matter at high densities. A Gibbs construct is used to describe the quark-hadron phase transition at large densities and at zero temperature. Within the model, as the density is increased, a mixed phase appears at about 2.5 times the nuclear matter saturation density (ρ0) and ends at about 5 ρ0 beyond which pure quark matter phase appear. It turns out that a stable hybrid star of maximum mass, M = 2.27 M with radius R = 14 km, can exist with a quark matter core in a mixed phase only. As the density decreases from the center to the surface, there is a sharp increase of the velocity of sound at the point where the quark-hadron phase transition occurs. This leads to the possibility of low frequency non-radial oscillations, the g modes, in hybrid stars in contrast to canonical neutron stars which do not have such quark matter core. The higher f modes frequencies of neutron stars get enhanced in the presence of quark matter core in hybrid stars. The magnitude of g mode frequencies decrease with increase the repulsive interaction in quark matter.

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