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26 #ifndef O2SCL_COLD_NSTAR_H
27 #define O2SCL_COLD_NSTAR_H
29 #include <o2scl/eos_had_base.h>
30 #include <o2scl/tov_solve.h>
31 #include <o2scl/tov_solve.h>
32 #include <o2scl/table.h>
33 #include <o2scl/fermion.h>
34 #include <o2scl/root_cern.h>
35 #include <o2scl/mroot_cern.h>
36 #include <o2scl/mroot_hybrids.h>
37 #include <o2scl/eos_tov.h>
39 #ifndef DOXYGEN_NO_O2NS
221 int fixed(
double target_mass);
373 #ifndef DOXYGEN_INTERNAL
399 std::shared_ptr<table_units<> >
eost;
409 #ifndef DOXYGEN_NO_O2NS
double acausal_pr
The pressure at which the EOS becomes acausal.
std::shared_ptr< table_units<> > eost
Storage for the EOS table.
double nb_start
The starting baryon density (default 0.05)
Naive static cold neutron star.
std::shared_ptr< table_units<> > get_eos_results()
Get the eos table (after having called calc_eos())
void set_eos_table(std::shared_ptr< table_units<> > t)
Return the results data table.
void set_eos(eos_had_base &he)
Set the equation of state.
int calc_eos(double np_0=0.0)
Calculate the given equation of state.
root * rp
A pointer to the solver.
double acausal
The density at which the EOS becomes acausal.
double allow_urca
The smallest density where Urca becomes allowed.
bool err_nonconv
If true, throw an exception if the solver fails or if the EOS is not well-formed (default true)
double pressure_dec
The smallest baryon density where the pressure starts to decrease.
bool include_muons
If true, include muons (default false)
double solve_fun(double x, thermo &hb)
Solve to ensure zero charge in -equilibrium.
eos_tov_interp def_eos_tov
Default EOS object for the TOV solver.
int calc_nstar()
Calculate the M vs. R curve.
root_cern def_root
The default equation solver for the EOS.
bool well_formed
If true, the energy density and pressure of the EOS is monotonically increasing and the pressure is a...
double acausal_ed
The energy density at which the EOS becomes acausal.
double nb_end
The final baryon density (default 2.0)
fermion pp
The default proton.
Class to solve the Tolman-Oppenheimer-Volkov equations.
bool eos_set
True if equation of state has been set.
int set_tov(tov_solve &ts)
Specify the object for solving the TOV equations.
std::shared_ptr< table_units<> > get_tov_results()
Get the results from the TOV (after having called calc_nstar())
int set_root(root<> &rf)
Set the equation solver for the EOS.
An EOS for the TOV solver using simple linear interpolation and an optional crust EOS.
int verbose
Verbosity parameter (default 0)
std::shared_ptr< table_units<> > get_results()
Return the results data table.
double solver_tol
Solver tolerance (default )
Hadronic equation of state [abstract base].
double barn
The baryon density.
double dnb
The baryon density stepsize (default 0.01)
fermion np
The default neutron.
int fixed(double target_mass)
Calculate the profile for a fixed gravitational mass.
tov_solve * tp
A pointer to the TOV object.
double calc_urca(double np_0=0.0)
Compute the density at which the direct Urca process is allowe.
fermion_zerot fzt
Zero-temperature fermion thermodynamics.
eos_had_base * hep
A pointer to the equation of state.
double deny_urca
The smallest density where Urca becomes disallowed.
tov_solve def_tov
The default TOV equation solver.
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