The phenomena of deconfinement hadronic matter into quark at high density, relevant to hybrid star (HS) cores, is studied in the present work. effective chiral model describes pure phase while for MIT bag chosen with density dependent pressure. Phase transition achieved using Maxwell construction. effect variation asymptotic value pressure ($B_{as}$) analyzed w.r.t mass and radius HSs. presence...

Abstract Given an Equation of State (EOS) for neutron star (NS) matter, there is a unique mass–radius sequence characterized by maximum mass M NS max at radius R max . ...

A kilonova signal is generally expected after a Black Hole - Neutron Star merger. The strength of the related to equation state neutron star matter and it increases with stiffness latter. recent results obtained by NICER from analyses PSR J0740+6620 suggest rather stiff therefore strong, at least if mass does not exceed $\sim 10 \mathrm{\,M}_\odot$ adimensional spin parameter too small orbit pr...

The current theoretical development identified as the gravitational decoupling via Complete Geometric Deformation (CGD) method that has been introduced to explore nonmetricity $Q$ effects in relativistic astrophysics. In present work, we have investigated gravitationally decoupled anisotropic solutions for strange star framework of $f(Q)$ gravity by utilizing CGD technique. To do this, started ...

Neutron stars are the densest objects in Universe, with M ∼ 1.4 M⊙ and R 12 km, equation of state associated to their internal composition is still unknown. The extreme conditions which matter subjected inside neutron could lead a phase transition inner cores, giving rise hybrid compact object. observation 2M⊙ binary pulsars (PSR J1614-2230, PSR J0343+0432 J0740+6620) strongly constraints theor...

Abstract Observations of optical and near-infrared counterparts binary neutron star mergers not only enrich our knowledge about the abundance heavy elements in universe help reveal remnant object just after merger, which is generally known, but can also effectively constrain dense properties nuclear matter equation state (EOS) interior merging stars. Following relativistic mean-field descriptio...

The distribution of the dark matter (DM) in DM-admixed-neutron stars (DANSs) is supposed to be either a dense core or an extended halo, which subject DM fraction DANS ($f_{\chi}$) and properties, such as mass ($m_{\chi}$) strength self-interaction ($y$). In this paper, we perform in-depth analysis formation criterion for core/dark halo point out that relative these two components essentially de...

The spacetime surrounding compact objects such as neutron stars and black holes provides an excellent place to study gravity in the strong, nonlinear, dynamical regime. Here, effects of strong curvature can leave their imprint on observables which we may use gravity. Recently, NICER provided a mass radius measurement isolated star using x-rays, while LIGO/Virgo measured tidal deformability thro...

Instead of parametrizing the pressure-density relation a neutron star (NS), one can parametrize its macroscopic properties such as mass ($M$), radius ($R$), and dimensionless tidal deformability ($\mathrm{\ensuremath{\Lambda}}$) to infer equation state (EOS) combining electromagnetic gravitational wave (GW) observations. We present new method $R(M)$ $\mathrm{\ensuremath{\Lambda}}(M)$ relations,...

In this paper, we employ one variant of the Generalized Uncertainty Principle (GUP) model, i.e., Kempf-Mangano-Mann (KMM) and discuss impact GUP on EoS nuclear neutron star matter based Relativistic Mean Field (RMF) model. We input result in Serrano-Li\v{s}ka (SL) gravity theory to corresponding Neutron Star (NS) properties. have shown that upper bound for parameter from properties is $\beta \l...