Abstract
The neutron star properties are generally determined by the equation of state of β-equilibrated dense matter. In this work, we consider the interaction of fermionic dark matter (DM) particles with nucleons via Higgs exchange and investigate the effect on the neutron star properties with the relativistic mean-field model equation of state coupled with DM. We deduce that DM significantly affects the neutron star properties, such as considerably reducing the maximum mass of the star, which depends on the percentage of the DM considered inside the neutron star. The tidal Love numbers both for electric and magnetic cases and surficial Love numbers are also studied for DM admixed NS. We observed that the magnitude of tidal and surficial Love numbers increases with a greater DM percentage. Further, we present post-Newtonian tidal corrections to gravitational waves decreased by increasing the DM percentage. The DM effect on the GW signal is significant during the late inspiral and merger stages of binary evolution for GW frequencies >500 Hz.
Highlights
Gravitational waves (GWs) are emitted from binary neutron star (BNS) mergers, such as GW170817 [1] and GW190425 [2]
The tidal deformability is expressed in terms of the gravitoelectric and gravitomagnetic Love numbers, and the surface deformation of the star is described by the surficial Love numbers
We calculated the macroscopic properties of NSs, such as the mass, radius and compactness, by solving the Tolman–Oppenheimer– Volkoff (TOV) equations as an input of the effective field-theorymotivated relativistic mean-field equation of states
Summary
Gravitational waves (GWs) are emitted from binary neutron star (BNS) mergers, such as GW170817 [1] and GW190425 [2]. GWs discoveries of BNS mergers can be a novel probe for nuclear physics as they encode information about the EOS in neutron-rich dense matter through finitesize effects and provide information on NS properties, such as the mass and tidal deformability [19,20,21,22,23,24,25,26,27,28,29,30,31,32]. [38] and analyse the results of the higher-order tidal Love numbers (electric-type and magnetic-type) and surficial love numbers of the NSs. With the increased sensitivity of upcoming third-generation GW detectors and gravitational-wave detection of BNS mergers, that analysis is potentially important [57,58]. We are analyse the tidal correction on the GWs emitted by BNS in the in-spiral phase
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