Radial modes of slowly rotating compact stars in the presence of magnetic field

Panda, Nandita; Mohanta, K K; Sahu, P. K.

doi:10.1140/epja/i2016-16286-7

Cited by 3 publications

(2 citation statements)

References 46 publications

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“…Our comprehension of the internal structure of an NS will surely be further deepened by a reasonable application of this study in more realistic environments considering rotation, non-zero temperature and magnetic fields [74]. Additionally, research on the potential for radial oscillation frequency detection and efforts to increase detector sensitivity will provide a chance for observational validation of our theory.…”

Section: Discussionmentioning

confidence: 84%

Radial Oscillations in Neutron Stars from Unified Hadronic and Quarkyonic Equation of States

et al. 2023

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We study radial oscillations in non-rotating neutron stars by considering the unified equation of states (EoSs), which support the 2 M⊙ star criterion. We solve the Sturm–Liouville problem to compute the 20 lowest radial oscillation modes and their eigenfunctions for a neutron star modeled with eight selected unified EoSs from distinct Skyrme–Hartree–Fock, relativistic mean field and quarkyonic models. We compare the behavior of the computed eigenfrequency for an NS modeled with hadronic to one with quarkyonic EoSs while varying the central densities. The lowest-order f-mode frequency varies substantially between the two classes of the EoS at 1.4 M⊙ but vanishes at their respective maximum masses, consistent with the stability criterion ∂M/∂ρc>0. Moreover, we also compute large frequency separation and discover that higher-order mode frequencies are significantly reduced by incorporating a crust in the EoS.

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Section: Discussionmentioning

confidence: 84%

Radial Oscillations in Neutron Stars from Unified Hadronic and Quarkyonic Equation of States

et al. 2023

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“…To investigate radial oscillations in newborn NSs after supernova explosions or the merger of NSs, the features of more realistic environments, e.g., temperature, rotation, and magnetic field, should also be included [89]. We leave these studies to future work, together with those employing other EOSs.…”

Section: Discussionmentioning

confidence: 99%

The equation of state and radial oscillations of neutron stars

Sun,

Zheng,

Chen

et al. 2021

Preprint

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We investigate radial oscillations of pure neutron stars and hybrid stars, employing equations of state of nuclear matter from Brueckner-Hartree-Fock theory, and of quark matter from the Dyson-Schwinger quark model, performing a Gibbs construction for the mixed phase in hybrid stars. We calculate the eigenfrequencies and corresponding oscillation functions. Our results for the zero points of the first-order radial oscillation frequencies give the maximum mass of stable neutron stars, consistent with the common criterion dM/dρ c = 0. Possible observations of the radial oscillation frequencies could help to learn more about the equation of state, predict the maximum mass of neutron stars more precisely, and indicate the presence of quark matter.

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