![]() ![]() Moment of inertia and its mass, then we demonstrate the insensitivity of theĭimensionless moment of inertia and normalized moment of inertia to the EoSs. To include slow rotation regime and determine the relation between the star's Most massive NS ever observed, PSR J0952-0607. With $ \xi=0.25 $ which is in close proximity to the recent discovery of the Of the GW170817 event and indicate a maximum mass of $2.37M_$ for BSk21 Ourįindings show a high degree of compatibility with the observational constraints ![]() The star employing a set of different realistic equations of state (EoSs). We plot the radial profiles of the metricįunctions and the scalar field as well as extracting the mass-radius diagram of Interior and exterior regions using the appropriate boundary conditions near Normally this will be a system with the origin at the particle and a horizontal x axis and a vertical. The particle will be the object or point where the lines of action of all the forces intersect. We derive the hydrostaticĮquilibrium equations in static case and solve them numerically for both The general procedure for solving equilibrium of a particle problems in two dimensions is to: Identify the particle. Through a coupling parameter $ \xi $ plus a potential of the form $ Scalar field $ \phi $ that is nonminimally coupled to the torsion scalar $ T $ On a particular type of theory $ F(T,\phi,X) $ which includes a canonical The framework of teleparallel gravity, namely scalar torsion theories. Static and slowly rotating neutron stars (NSs) in scalar tensor theories within Download a PDF of the paper titled Neutron Stars in Scalar Torsion Theories with Nonminimal Coupling, by Youcef Kehal and 1 other authors Download PDF Abstract: The aim of this paper is to investigate the existence and the structure of
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