Procedures

This SUBROUTINE allocates a polymorphic object of class idbase to its dynamic type. The dynamic type is one among those that interpolate the ID from a grid

This SUBROUTINE allocates a polymorphic object of class idbase to its dynamic type. The dynamic type is one among those that use the \(\texttt{FUKA}\) \(\mathrm{ID}\)

This SUBROUTINE allocates a polymorphic object of class idbase to its dynamic type. The dynamic type is one among those that use the \(\texttt{LORENE}\) \(\mathrm{ID}\)

This SUBROUTINE allocates a polymorphic object of class idbase to its dynamic type. The dynamic type is one among all the supported \(\mathrm{ID}\)

Assign a mass to each surface, based on the radial mass profile of the star (computed along the larger equatorial radius)

Compute the Cartesian coordinates of a points $p$, starting from the spherical, or optionally elliptical, polar coordinates of the point $p$ relative to a point $O$

Compute the colatitudes according to a uniform distribution over a surface, between alpha and beta, with pi/2 < alpha < beta < pi. The values are stored in the array colatitudes See https://mathworld.wolfram.com/SpherePointPicking.html

Generic PROCEDURE to compute the Cauchy convergence factor

Computes the spacetime metric from lapse, shift and spatial metric

Computes the Landau-Lifshitz pseudotensor on the mesh, using the definition in eq.(96.9) in Landau and Lifshitz, The Classical Theory of Fields, Pergamon Press(1975)

Computes the lapse,shift and spatial metric from the covariant spacetime metric

Compute the determinant of a $3\times 3$ symmetric matrix field, given as a 6-vector, at a given grid point

Compute the determinant of a $4\times 4$ symmetric matrix field, given as a 10-vector

Function used in the computation of the degenerate pressure

Backup method to find the smoothing length via brute force if the optimized method gives 0. It sets the smoothing lengths to the distance between the particle and the ndes-th closest neighbour.

Generic PROCEDURE to compute the grid points shared by all the grids used to perform a Cauchy convergence test

Function used in the computation of the degenerate specific internal energy

Wrapper SUBROUTINE to get the value of the Hamiltonian constraint computed using ID read on the refined mesh, at a given mesh point (i,j,k), on the refinement level l, for the tpo object tpof

Wrapper SUBROUTINE to get the value of the Hamiltonian constraint computed using using the hydro ID mapped from the particles to the refined mesh, at a given mesh point (i,j,k), on the refinement level l, for the tpo object tpof

Invert a $3\times 3$ symemtric matrix stored as a $6$-vector

Invert a $4\times 4$ symemtric matrix stored as a $10$-vector

Test if a double precision is a finite number

Compute the constant to convert the polytropic constant $K$ from the units used in \(\texttt{LORENE}\) for the single polytropic \(\mathrm{EOS}\), to the units used in \(\texttt{SPHINCS}\)

Compute the constant to convert the polytropic constant $K$ from the units used in \(\texttt{LORENE}\) for the piecewise polytropic \(\mathrm{EOS}\), to the units used in \(\texttt{SPHINCS}\)

Compute the Newtonian energy and angular momentum of the system, imposing that the radial velocity of the fictitious body is 0 at the desired periastron, with the desired eccentricity.

Compute Newtonian speeds for two stars on parabolic orbits at a given distance, applying conservation of energy and momentum. For a 2-body problem with parabolic orbit, the total energy is zero.

Compute the number of surfaces by integrating the linear particle density along the larger equatorial radius

Compute the geometrical particle volume not the proper particle volume.

Interface of TYPE particles

Generic PROCEDURE to perform the Cauchy convergence test

Place the surfaces, according to the baryon mass density of the star along the larger equatorial radius

Degenerate pressure as a function of density

Degenerate pressure as a function of density, all in CGS units

Print the Cauchy convergence factor to a formatted file

Print star's radial mass profile and radii of surfaces to different ASCII files

Read the two BSSN TOV ID files produced with setup_TOV.x, and place them symmetrically on the $x$ axis so that their distance is equal to the periastron given as input

Read the \(\mathrm{CompOSE}\) files *.thermo.ns, *.nb.ns, containing the $\beta$-equilibrated \(\mathrm{EOS}\) computed by the \(\mathrm{CompOSE}\) software.

Read the parameters to steer SPHINCS_ID

Read the two SPH TOV ID files produced with setup_TOV.x, and place them symmetrically on the $x$ axis so that their distance is equal to the periastron given as input

Reallocate a 1-dimensional array

Reallocate a 2-dimensional array

Degenerate density as a function of pressure

Test if a double precision is a finite number

Test if a double precision is a finite number

Compute the spacetime squared norm of a vector, using the metric given as an array of 10 components

Compute the spatial squared norm of a vector, using the spatial metric given as an array of 6 components

Compute the spherical polar coordinates of a point $p$ relative to a point $O$, starting from the Cartesian coordinates of the points $p$ and $O$

Compute the BSSN variables starting from the standard 3+1 (aka ADM) variables This is basically a version of ADM_to_BSSN from MODULE McLachlan_refine that allows for array arguments.

Test if a status variable is 0 or not

Test that the implementation is correct. Takes the density in code units as input, and assigns CGS values to the pressure, and the density recomputed from the pressure. It also computed the dimensionless specific internal energy.

Degenerate specific internal energy as a function of density

Write the components of symmetric $3\times 3$ matrix given as a $6$-vector, into a $3\times 3$ matrix