Numerical code and data for the stellar structure and dynamical instability analysis of generalised uncertainty white dwarfs

The enclosed code and dataset correspond to the numerical solution of  Tolman Oppenheimer Volkoff (TOV) equation (3.3) and (3.4) and the dynamical instability scheme given by equations 4.13 to 4.16 in the research article ``Existence of Chandrasekhar's limit in generalized uncertainty white dwarfs'' by the same authors. The dataset is generated for a wide range of central Fermi momentum $xi_c$ supplemented by the equation of state (2.6) and (2.11)  parametrized by the Fermi momentum $\xi$. For a given value of central Fermi momentum, the solution gives the total mass and radius of the white dwarfs. These solutions facilitate the evaluation of the integrals 4.14--4.16 giving the eigenfrequency of the fundamental mode in equation (4.13).

Methods
The research article entitled ``Existence of Chandrasekhar's limit in generalized uncertainty white dwarfs'' by the same authors requires a numerical solution of the Einstein equation for spherically symmetric white dwarf stars.  

A single dataset in Figures (1) and (2) in the research article corresponds to solving Tolman Oppenheimer Volkoff (TOV) equations for a range central Fermi momenta with a particular choice of GUP parameter $\beta_0$. The first-order differential equations (see equations 3.3 and 3.4 in the article) are solved numerically with the aid of C programming using the fourth-order Runge-Kutta method with boundary conditions as described in the article. 

The dataset for the eigenfrequency of the fundamental mode is obtained from the dynamical instability scheme as described in the article. Integrations in equations 4.14-4.16 carried out employing the Trapezoidal method. This yields the eigenfrequency corresponding to a range of central Fermi momentum (or central density) for a particular choice of the GUP parameter $\beta_0$.