Equation of state of asymmetric nuclear matter using re-projected nucleon–nucleon potentials

Abstract

In this paper, we have calculated the equation of state of asymmetric nuclear matter using the lowest order constrained variational approach and Argonne family potentials with and without three-nucleon interaction(TNI) contribution. In particular, we have used the AV18 potential and the re-projected potentials, AV8′, and AV6′. We have also calculated the saturation properties of symmetric nuclear matter, and the nuclear symmetry energy using AV18 +TNI, AV8′+TNI and AV6′+TNI potentials. The inclusion of TNI has modified the agreement with experiment. We have also made a comparison between our results and those of other many-body calculations.

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.…”

“…In this formalism, the trial wave function in the form of ψ = F φ is adopted in which φ and F = S i>j f (ij) correspond to the slater determinant of A independent nucleons and Jastrow form of A-body correlation operator with S being a symmetrizing operator, respectively. It is to be noted that the two-body energy consists of two-body correlation operator f (12) [26] and two-body potential V (12), which the Argonne family potentials, namely AV6 ′ +TNI, AV8 ′ +TNI, and AV18+TNI [22] are considered in this study. Here, TNI refers to the three-nucleon interaction contribution [27].…”

“…Moreover, the threshold density ρ th at which kaons appear can be calculated through these equations for θ = 0. Table I presents our results for incompressibility coefficient and symmetry energy at saturation density, its slope [22], and also the threshold density for candidate EoSs in addition to those obtained from the EoS with AV18 potential in [21]. Very recently, symmetry energy constraints have been obtained to be 42 < L < 117 MeV and 32.5 < S 0 < 38.1 MeV applying ratios of the charged pion spectra [30].…”

“…In this work, we also intend to explore the effect of kaon condensation on our previously obtained results for the mass-radius relation of NSs [22] in addition to their tidal deformability in a binary neutron star merger and check the validity of our calculations with the observational constraints.…”

Studying VLOCV twin compact stars with binary mergers

“…In general, this model makes the EoS so stiff that the maximum mass of the neutron star increases substantially. In addition, we consider an EoS [30] that features the three nucleon interaction (TNI) for the sake of comparison. At the same time, the constant speed of sound (CSS) parametrization is utilized for the high-density region considering the first order phase transition from hadronic matter to quark matter.…”