Class ex_eos_had_apr

O2scl_eos : Class List

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.

const int low_phase = 1
const int mixed_phase = 2
const int high_phase = 3
int maxwell_fig7(size_t nv, const ubvector &x, ubvector &y)

Function for the Maxwell construction in Fig. 7.

int mixedmaxwell(size_t nv, const ubvector &x, ubvector &y)

Maxwell construction of the nuclear matter mixed phase.

int fig7fun(size_t nv, const ubvector &x, ubvector &y)

Function to construct Fig. 7.

int nstar_low(size_t nv, const ubvector &x, ubvector &y)

Solve for neutron star matter (low-density phase)

int nstar_high(size_t nv, const ubvector &x, ubvector &y)

Solve for neutron star matter (high-density phase)

int nstar_mixed(size_t nv, const ubvector &x, ubvector &y)

Solve for neutron star matter (mixed phase)

void store_data()

Write a line of data to the table.

int nucmixed(size_t nv, const ubvector &x, ubvector &y)

Solve for nuclear matter (mixed phase)

int neutmixed(size_t nv, const ubvector &x, ubvector &y)

Solve for neutron matter (mixed phase)

int nucleimat(size_t nv, const ubvector &ex, ubvector &ey)

Solve for phase transition to nuclei.

int nucleimat_pdrip(size_t nv, const ubvector &ex, ubvector &ey)

Solve for phase transition to nuclei with a proton drip.

ex_eos_had_apr()
void run()

Main driver, computing the APR EOS and the associated M vs. R curve.