Tidal deformability of binary neutron stars employing equation of state with LOCV approach

Abstract

The tidal deformability of binary neutron stars (BNSs) and their structural properties are calculated applying different equations of state (EOSs), obtained from the lowest order constrained variational many-body theory. Therefore, potentials such as AV8′, AV6′ with and without three-nucleon interaction (TNI), AV18+TNI, and UV14+TNI are employed in order to investigate the properties of neutron stars (NSs) in coalescing binary systems. The same EOS is considered for the individual component of the merger in addition to the low spin prior case. We determine the value of dimensionless tidal deformability Λ in the range of 216 < Λ < 314 regarding 1.4 M⊙ configuration of NS with the EOSs of Argonne family potentials and UV14 accompanied by TNI. Our obtained results are in good consistency with the very recent observation of the BNS merger GW170817. It is figured out that most of the applied EOSs are in the vicinity of the 50% credible region of the PhenomPNRT and TaylorF2 waveform models. Moreover, the effect of the outer and inner crust on the EOS is studied so that we find out that the tidal Love number has the largest value without the contribution of the outer crust considering the particular example of 1.4 M⊙ configuration of NSs.

Binary neutron star mergers within kaon condensation:GW170817

“…In figure 3 Furthermore, the results obtained for the EoSs without kaon condensation, which have been discussed in our previous works [22,31], are presented by solid black lines in this figure. It can be noticed that in this figure, the kaon condensation with all values of a 3 m s results in the reduction of pressure, in particular for the densities close to the threshold density and also lower amounts of a 3 m s .…”

Binary neutron star mergers within kaon condensation: GW170817

“…However, AV6'+TNI potential results in higher kaon fraction compared to other potentials in both strangeness values. Furthermore, the results obtained for the EoSs without kaon condensation, which have been discussed in our previous works [22,31], are presented by solid black lines in this figure . It can be noticed that in this figure, the kaon condensation with all values of a 3 m s results in the reduction of pressure, in particular for the densities close to the threshold density and also lower amounts of a 3 m s . On the other hand, the softening of the EoSs takes place in the whole range of density for all values of strangeness except a 3 m s =-310 MeV for the AV6 ′ +TNI case, which stiffens the EoS at the end of the density range.…”

Studying VLOCV twin compact stars with binary mergers

“…In our previous work [60], we have computed the tidal deformability of binary neutron stars with four distinctive EoSs without phase transition, which the EoS of AV 18 +TNI resulted in better outcome compared to other ones. Therefore, we have selected this EoS in order to draw a comparison between the nucleon size and TNI, which is presented in Fig.…”