Effects of dark matter on the in-spiral properties of the binary neutron stars
arXiv:2104.01815 · doi:10.1093/mnras/stab2387
Abstract
Using the relativistic mean-field model, we calculate the properties of binary neutron star (BNS) in the in-spiral phase. Assuming the dark matter (DM) particles are accreted inside the neutron star (NS) due to its enormous gravitational field, the mass , radius , tidal deformability and dimensionless tidal deformability are calculated at different DM fractions. The value of , , and decreases with the increase of DM percentage inside the NS. The in-spiral phase properties of the BNS are explored within the post-Newtonian (PN) formalism, as it is suitable up to the last orbits in the in-spiral phase. We calculate the strain amplitude of the polarization waveform and , (2,2) mode waveform , orbital phase , frequency of the gravitational wave and PN parameter with DM as an extra candidate inside the NS. The magnitude of , and are almost the same for all assumed forces; however, the in-spiral time duration in the last orbit is different. We find that the BNS with soft equation of state and a high fraction of DM sustains more time in their in-spiral phase. We suggest that one should take DM inside the NS when they modelling the in-spiral waveforms for the BNS systems.
arXiv comment9 pages, 7 figures, 2 tables, accepted for publication in MNRAS
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