Tutorials

This test follows the computation focusses on the computation of a non-barotropic configuration

For a careful theoretical understanding, one has to investigate the exact model parameters that are employed. The equation of state follows the form (Eq. 45 of Camelio et al., 2019):

with the thermal barotropic law

and the rotational barotropic law (Eq. 24 of Camelio et al., 2019)

with (Eq. 38 of Camelio et al., 2019)

The simple example that is given in the git repository looks at a cold, rigidly rotating neutron star. In input parameters can be found at the beginning of kepler.f90 and they are:

• gam (double) –> polytropic index of the cold component
• gamth (double) –> exponent of the thermal component
• k1 (double) –> proportionality constant of the cold component
• k2 (double) –> proportionality constant of the thermal component
• k3 (double) –> entropy proportionality constant of the barotropic law
• omg0 (double) –> angular velocity in the center
• bvalue (double) –> baroclinic parameter
• rho0 (double) –> central rest mass density
• sigma (double) –> inverse scale radius of the differential rotation sigma = 1/R0
• verbose (logical) –> determines if output is put on the screen
• logfile (character) –> defines where the extended summary of the results is stored
• binfile (character) –> defined where the stellar profiles are stored
• maxit (integer) –> maximum number of iterations for the Newton-Raphson scheme
• tol (double) –> relative tolerance of the employed Newton-Raphson scheme
• relax_iters (integer) –> relaxation iterations in the force balance equation (Euler) solver
• rhocit (double) –> critical density for the EOS inversion from (p, hden) to (rho, s)
• funmax (double) –> maximal value of the function needed for the EOS inversion from (p, hden) to (rho, s)

After following the outlined installation guide, you can run a first test configuration

./nobarotropic.x