Compute the APR EOS with a Gibbs construction and the mass versus radius curve [Example class]. More...
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.
Definition at line 62 of file ex_eos_had_apr.cpp.
Protected Attributes | |
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 |
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. More... | |
|
inline |
Compute matter at densities below the maxwell construction
Definition at line 608 of file ex_eos_had_apr.cpp.
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