REVIEW 2 cited by
Gravitational wave asteroseismology of dark matter hadronic stars
Not yet reviewed by Pith; the record is open.
This paper has not been read by Pith yet. Machine review is queued; the pith claim, tier, and objections will appear here once it completes.
SPECIMEN: schema-true, not a live event
T0 review · schema-true
One-sentence machine reading of the paper's core claim.
pith:XXXXXXXX · record.json · timestamp
abstract
The influence of the dark matter mass~($M_{\chi}$) and the Fermi momentum~($k_{F}^{\dm}$) on the $f_0$-mode oscillation frequency, damping time parameter, and tidal deformability of hadronic stars are studied by employing a numerical integration of hydrostatic equilibrium, nonradial oscillation, and tidal deformability equations. The matter inside the hadronic stars follows the NL3* equation of state. We obtain that the influence of $M_{\chi}$ and $k_F^{\dm}$ is observed in the $f_0$-mode, damping tome parameter, and tidal deformability. Finally, the correlation between the tidal deformability of the GW$170817$ event with $M_{\chi}$ and $k_F^{\dm}$ are also investigated.
Forward citations
Cited by 2 Pith papers
-
Examining the influence of anisotropy on the fundamental mode of nonradial oscillation in neutron stars on a complete general relativistic scheme
Pressure anisotropy in strange quark stars measurably changes the f-mode oscillation frequency and the dimensionless tidal deformability, with positive anisotropy increasing mass and deformability while lowering the f...
-
Effect of Dark matter and $\sigma$-cut potential on radial and non-radial oscillation modes in neutron stars
Dark matter-admixed neutron stars oscillate at higher f- and p1-mode frequencies than ordinary or σ-cut models, while quasi-universal oscillation relations still hold.
Discussion (0). Sign in to comment.