def profile(eos,
energy_center,
number=200,
initr=0.001,
energy_0=1e7,
rad_0=False):
'''Calculate the enthalpy profile of a neutron star with equation of
state eos and central energy density energy_center in g/cm^3
optional arguments:
number: number of points
initr: size of central seed
energy_0: energy density at which to stop resolving crust. This doesn't
need to be tiny (and may cause problems if it is). Integration still
goes to surface.
rad_0: Set true to calculate outer radius at energy_0 instead of at
formal zero enthalpy limit of EOS
'''
# set up a core with small initial radius and mass
initm = 4.0 / 3.0 * np.pi * (initr)**3 * energy_center * Gcc
init_rm = np.array([initr, initm])
# central enthalpy
enth_c = eos.enthalpy(energy_center)
# end the core spacing here
enth_0 = eos.enthalpy(energy_center / 10)
# resolve core with linear spacing in enthalpy
linenths = np.linspace(enth_c, enth_0, number / 2)[:-1]
# end the crust spacing here and jump to 0
enth_0 = eos.enthalpy(energy_0)
# resolve crust with log spacing in enthalpy
logenths = np.logspace(np.log10(linenths[-1]), np.log10(enth_0),
number / 2 + 1)[1:]
# set of enthalpies to calculate energy density, radius, and mass at
if rad_0:
enths = np.hstack((np.array(linenths), np.array(logenths)))
else:
enths = np.hstack(
(np.array(linenths), np.array(logenths), np.array(0)))
# enths = np.linspace(enth_c, 0, number) # boring way for debugging
# integrate the TOV equations specified in deriv above
rms = integrate.odeint(deriv, init_rm, enths, args=(eos, ))
return np.vstack((enths, np.transpose(rms)))
def profile(eos, energy_center , number=200, initr=0.001, energy_0=1e7,
rad_0=False):
'''Calculate the enthalpy profile of a neutron star with equation of
state eos and central energy density energy_center in g/cm^3
optional arguments:
number: number of points
initr: size of central seed
energy_0: energy density at which to stop resolving crust. This doesn't
need to be tiny (and may cause problems if it is). Integration still
goes to surface.
rad_0: Set true to calculate outer radius at energy_0 instead of at
formal zero enthalpy limit of EOS
'''
# set up a core with small initial radius and mass
initm = 4.0/3.0*np.pi*(initr)**3 * energy_center * Gcc
init_rm = np.array([initr,initm])
# central enthalpy
enth_c = eos.enthalpy(energy_center)
# end the core spacing here
enth_0 = eos.enthalpy(energy_center/10)
# resolve core with linear spacing in enthalpy
linenths = np.linspace(enth_c, enth_0, number/2)[:-1]
# end the crust spacing here and jump to 0
enth_0 = eos.enthalpy(energy_0)
# resolve crust with log spacing in enthalpy
logenths = np.logspace(np.log10(linenths[-1]),np.log10(enth_0),
number/2+1)[1:]
# set of enthalpies to calculate energy density, radius, and mass at
if rad_0:
enths = np.hstack((np.array(linenths),np.array(logenths)))
else:
enths = np.hstack((np.array(linenths),np.array(logenths),np.array(0)))
# enths = np.linspace(enth_c, 0, number) # boring way for debugging
# integrate the TOV equations specified in deriv above
rms = integrate.odeint(deriv, init_rm, enths, args=(eos,))
return np.vstack((enths,np.transpose(rms)))
def rotprofile(eos, energy_center, number=100, initr=0.001, energy_0=1e7):
'''Calculate the enthalpy profile of a slowly rotating neutron star with
equation of state eos and central energy density energy_center in g/cm^3.
optional arguments:
number: number of points
initr: size of central seed
energy_0: energy density at which to stop resolving crust. This doesn't
need to be tiny (and may cause problems if it is). Integration still
goes to surface.
'''
#TODO: consolodate the profile functions; this mostly just repeats
#profile but with different initial conditions
# central enthalpy and density
enth_c = eos.enthalpy(energy_center)
dens_c = eos.density(enth_c)
# set up a core with small initial radius and mass
initm = 4.0 / 3.0 * np.pi * (initr)**3 * energy_center * Gcc
initma = 4.0 / 3.0 * np.pi * (initr)**3 * dens_c * Gcc
init_rm = np.array([initr, initm, initma, 0.0, 1.0])
# resolve core with linear spacing
linenths = np.linspace(enth_c, enth_c / 10, number)[:-1]
# resolve crust with log enth spacing
enth_0 = eos.enthalpy(energy_0) # end the crust spacing here and jump to 0
logenths = np.logspace(np.log10(linenths[-1]), np.log10(enth_0),
number / 2 + 1)
# set of enthalpies to calculate energy density, radius, and mass at
enths = np.hstack(
(np.array(linenths), np.array(logenths[1:]), np.array(0)))
# enths = np.linspace(enth_c, 0, number) # boring way for debugging
# integrate the TOV equations specified in deriv above
rms = integrate.odeint(rotderiv, init_rm, enths, args=(eos, ))
return np.vstack((enths, np.transpose(rms)))
def rotprofile(eos, energy_center , number=100, initr=0.001, energy_0=1e7):
'''Calculate the enthalpy profile of a slowly rotating neutron star with
equation of state eos and central energy density energy_center in g/cm^3.
optional arguments:
number: number of points
initr: size of central seed
energy_0: energy density at which to stop resolving crust. This doesn't
need to be tiny (and may cause problems if it is). Integration still
goes to surface.
'''
#TODO: consolodate the profile functions; this mostly just repeats
#profile but with different initial conditions
# central enthalpy and density
enth_c = eos.enthalpy(energy_center)
dens_c = eos.density(enth_c)
# set up a core with small initial radius and mass
initm = 4.0/3.0*np.pi*(initr)**3 * energy_center * Gcc
initma = 4.0/3.0*np.pi*(initr)**3 * dens_c * Gcc
init_rm = np.array([initr,initm, initma, 0.0, 1.0])
# resolve core with linear spacing
linenths = np.linspace(enth_c, enth_c/10, number)[:-1]
# resolve crust with log enth spacing
enth_0 = eos.enthalpy(energy_0) # end the crust spacing here and jump to 0
logenths = np.logspace(np.log10(linenths[-1]),np.log10(enth_0),
number/2+1)
# set of enthalpies to calculate energy density, radius, and mass at
enths = np.hstack((np.array(linenths),np.array(logenths[1:]),np.array(0)))
# enths = np.linspace(enth_c, 0, number) # boring way for debugging
# integrate the TOV equations specified in deriv above
rms = integrate.odeint(rotderiv, init_rm, enths, args=(eos,))
return np.vstack((enths,np.transpose(rms)))