Class ex_eos_had_apr¶
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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
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fermion_zerot
fzt
¶ Compute zero-temperature thermodynamics.
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fermion
n
¶ Neutron for low-density phase.
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fermion
p
¶ Proton for low-density phase.
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fermion
n2
¶ Neutron for high-density phase.
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fermion
p2
¶ Proton for high-density phase.
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fermion
e
¶ Electron for low-density phase.
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fermion
mu
¶ Muon for low-density phase.
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fermion
e2
¶ Electron for high-density phase.
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fermion
mu2
¶ Muon for high-density phase.
‘Thermo’ objects
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thermo
hb
¶ Baryon thermodynamics for low-density phase.
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thermo
l
¶ Leptonic thermodynamics for low-density phase.
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thermo
hb2
¶ Baryon thermodynamics for high-density phase.
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thermo
tot
¶ Total thermodynamics.
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thermo
l2
¶ Leptonic thermodynamics for high-density phase.
Numerical methods
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mroot_hybrids
solver
¶ General solver.
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mroot_hybrids
solver_trans_density
¶ Solver for transition densities (lower tolerances)
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deriv_cern
cd
¶ Derivative object.
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double
nb
¶ Baryon density.
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double
chi
¶ Volume fraction of low-density phase.
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double
mub
¶ Baryon chemical potential.
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double
muq
¶ Charge chemical potential.
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double
f7x
¶ Proton fraction for Fig. 7.
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int
choice
¶ Choice of model from APR.
Phase specification
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int
phase
¶
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eos_had_apr
ap
¶ Base APR EOS.
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table_units
at
¶ Table for output.
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hdf_file
hf
¶ HDF file for output.
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const int
low_phase
= 1¶
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const int
mixed_phase
= 2¶
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const int
high_phase
= 3¶
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int
maxwell_fig7
(size_t nv, const ubvector &x, ubvector &y)¶ Function for the Maxwell construction in Fig. 7.
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int
mixedmaxwell
(size_t nv, const ubvector &x, ubvector &y)¶ Maxwell construction of the nuclear matter mixed phase.
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int
fig7fun
(size_t nv, const ubvector &x, ubvector &y)¶ Function to construct Fig. 7.
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int
nstar_low
(size_t nv, const ubvector &x, ubvector &y)¶ Solve for neutron star matter (low-density phase)
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int
nstar_high
(size_t nv, const ubvector &x, ubvector &y)¶ Solve for neutron star matter (high-density phase)
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int
nstar_mixed
(size_t nv, const ubvector &x, ubvector &y)¶ Solve for neutron star matter (mixed phase)
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void
store_data
()¶ Write a line of data to the table.
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int
nucmixed
(size_t nv, const ubvector &x, ubvector &y)¶ Solve for nuclear matter (mixed phase)
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int
neutmixed
(size_t nv, const ubvector &x, ubvector &y)¶ Solve for neutron matter (mixed phase)
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int
nucleimat
(size_t nv, const ubvector &ex, ubvector &ey)¶ Solve for phase transition to nuclei.
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int
nucleimat_pdrip
(size_t nv, const ubvector &ex, ubvector &ey)¶ Solve for phase transition to nuclei with a proton drip.
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ex_eos_had_apr
()¶
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void
run
()¶ Main driver, computing the APR EOS and the associated M vs. R curve.
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fermion_zerot