Aims. We calculate parameters A and B of the Baym-Pines model of the hydro-elastic equilibrium of rotating neutron stars. Parameter A determines the energy increase of a non-rotating star due to a quadrupolar deformation of its shape. Parameter B determines residual quadrupolar deformation due to the crustal shear strain, in a neutron star that spun-down to a non-rotating state. Methods. The ca...

in this study we produced a new method for solving regular dierential equations with step size h and taylor series. this method analyzes a regular dierential equation with initial values and step size h. this types of equations include quadratic and cubic homogenous equations with constant coecients and cubic and second- level equations.

in this work, we proposed an efective method based on cubic and pantic b-spline scaling functions to solve partial differential equations of frac- tional order. our method is based on dual functions of b-spline scaling func- tions. we derived the operational matrix of fractional integration of cubic and pantic b-spline scaling functions and used them to transform the mentioned equations to a ...

Aims. We calculate parameters A and B of the Baym-Pines model of the hydro-elastic equilibrium of rotating neutron stars. Parameter A determines the energy increase of a non-rotating star due to a quadrupolar deformation of its shape. Parameter B determines residual quadrupolar deformation due to the crustal shear strain in a neutron star that spun down to a non-rotating state. Methods. The cal...

Ab initio methods using weakly interacting nucleons give a good description of condensed nuclear matter up to densities comparable the saturation density. At higher palpable strong interactions between overlapping become important; we propose that will continuously switch over follow holographic model in this region. In order implement this, construct hybrid equations state (EoSs) where various...

We revisit the extended Zimanyi-Moszkowski (EZM) model of dense neutron star (NS) core matter. In contrast to our previous work we treat the vector potentials of baryons on an equal footing with the e¤ective masses, and solve a set of 6 equations to determine the three independent e¤ective masses and vector potentials and a set of 2 equations to determine the conditions of -equilibrated NS matt...

The system of equations $$\begin{aligned}&u_1p_1^2 + \cdots u_sp_s^2 = 0,\\&v_1p_1^3 v_sp_s^3 0 \end{aligned}$$ has prime solutions $$(p_1, \ldots , p_s)$$ for $$s \ge 12$$ assuming that the modulo each p. This is proved via Hardy–Littlewood circle method, building on Wooley’s work corresponding over integers and recent results Vinogradov’s mean value theorem. Additionally, a set sufficient ...