Class ex_eos_had_apr ()¶

class ex_eos_had_apr¶

Compute the APR EOS with a Gibbs construction and the mass versus radius curve [Example class].

In succession, calculates nuclear matter, neutron matter, and then neutron star matter with Maxwell and Gibbs constructions.

We could use the more accurate masses in o2scl/constants.h here, but APR appears to have been designed to be used with neutron and protons masses equal to 939 MeV.

Fermions

fermion_zerot fzt¶: Compute zero-temperature thermodynamics.

fermion n¶: Neutron for low-density phase.

fermion p¶: Proton for low-density phase.

fermion n2¶: Neutron for high-density phase.

fermion p2¶: Proton for high-density phase.

fermion e¶: Electron for low-density phase.

fermion mu¶: Muon for low-density phase.

fermion e2¶: Electron for high-density phase.

fermion mu2¶: Muon for high-density phase.

‘Thermo’ objects

thermo hb¶: Baryon thermodynamics for low-density phase.

thermo l¶: Leptonic thermodynamics for low-density phase.

thermo hb2¶: Baryon thermodynamics for high-density phase.

thermo tot¶: Total thermodynamics.

thermo l2¶: Leptonic thermodynamics for high-density phase.

Numerical methods

mroot_hybrids solver¶: General solver.

mroot_hybrids solver_trans_density¶: Solver for transition densities (lower tolerances)

deriv_cern cd¶: Derivative object.

double nb¶: Baryon density.

double chi¶: Volume fraction of low-density phase.

double mub¶: Baryon chemical potential.

double muq¶: Charge chemical potential.

double f7x¶: Proton fraction for Fig. 7.

int choice¶: Choice of model from APR.

Phase specification

int phase¶

eos_had_apr ap¶: Base APR EOS.

table_units at¶: Table for output.

hdf_file hf¶: HDF file for output.

static const int low_phase = 1¶

static const int mixed_phase = 2¶

static const int high_phase = 3¶

inline int maxwell_fig7(size_t nv, const ubvector &x, ubvector &y)¶: Function for the Maxwell construction in Fig. 7.

inline int mixedmaxwell(size_t nv, const ubvector &x, ubvector &y)¶: Maxwell construction of the nuclear matter mixed phase.

inline int fig7fun(size_t nv, const ubvector &x, ubvector &y)¶: Function to construct Fig. 7.

inline int nstar_low(size_t nv, const ubvector &x, ubvector &y)¶: Solve for neutron star matter (low-density phase)

inline int nstar_high(size_t nv, const ubvector &x, ubvector &y)¶: Solve for neutron star matter (high-density phase)

inline int nstar_mixed(size_t nv, const ubvector &x, ubvector &y)¶: Solve for neutron star matter (mixed phase)

inline void store_data()¶: Write a line of data to the table.

inline int nucmixed(size_t nv, const ubvector &x, ubvector &y)¶: Solve for nuclear matter (mixed phase)

inline int neutmixed(size_t nv, const ubvector &x, ubvector &y)¶: Solve for neutron matter (mixed phase)

inline int nucleimat(size_t nv, const ubvector &ex, ubvector &ey)¶: Solve for phase transition to nuclei.

inline int nucleimat_pdrip(size_t nv, const ubvector &ex, ubvector &ey)¶: Solve for phase transition to nuclei with a proton drip.

inline ex_eos_had_apr()¶

inline void run()¶: Main driver, computing the APR EOS and the associated M vs. R curve.