Solve TOV Equation

Function to solve the TOV equation from EOS equation of state given by user.

TOVsolver.solver_code.TOV_def(r, y, inveos, ad_index)[source]

a function that packing the whole TOV equations set

Parameters:

  • r (float) – raius as integrate varible

  • y (psudo-varible) – containing pressure, mass, h and b as intergarte varibles

  • equation (to solve out the TOV)

  • inveos – the invert of the eos, pressure and energy density relation to integrate

  • interpolate. (and)

Returns:

The array that contains all the Stars’ masses, in M_sun as a Units. Radius (array): The array that contains all the Stars’s radius, in km. Tidal Deformability (array): The array that contains correpsonding Tidal property, These are dimension-less.

Return type:

Mass (array)

TOVsolver.solver_code.m1_from_mc_m2(mc, m2)[source]

a function that feed back the companion star mass from GW event measurement.

Parameters:

  • mc (float) – chrip mass of a GW event, unit in solar mass.

  • m2 (float or numpy array) – the determined mass for one of the star, this

  • EoS. (is computed from sampling of)

Returns:

the companion star mass in solar mass.

Return type:

m1 (float or numpy array)

TOVsolver.solver_code.solveTOV(center_rho, Pmin, eos, inveos)[source]

Solve TOV equation from given Equation of state in the neutron star core density range

Parameters:

  • center_rho (array) – This is the energy density here is fixed in main

  • [10**14.3 (that is range)

  • unit.g_cm_3 (10**15.6] *)

  • Pmin (float) – In unit.G / unit.c**4

  • eos (function) – pressure vs. energy density, energy density in unit.G / unit.c**2, pressure in unit.G / unit.c**4

  • inveos (function) – energy density vs. pressure

Returns:

The Stars’ masses Radius (float): The Stars’s radius

Return type:

Mass (float)

TOVsolver.solver_code.solveTOV_tidal(center_rho, energy_density, pressure)[source]

Solve TOV equation from given Equation of state in the neutron star core density range

Parameters:

  • center_rho (array) – This is the energy density here is fixed in main

  • np.logspace (that is)

  • energy_density (array) – Desity array of the neutron star EoS, in MeV/fm^{-3}

  • simiplicity (Notice here for)

  • magnitude (we omitted G/c**4)

  • so

  • MeV/fm^{-3})*G/c**4 ((value in)

  • are (could convert to the energy density we)

  • using

  • magnitude. (please check the Test_EOS.csv to double check the order of)

  • pressure (array) – Pressure array of neutron star EoS, also in nautral unit

  • MeV/fm^{-3} (with)

  • Test_EOS.csv (still please check the)

  • is (the conversion)

  • dyn/cm3)*G/c**4. ((value in)

Returns:

The array that contains all the Stars’ masses, in M_sun as a Units. Radius (array): The array that contains all the Stars’s radius, in km. Tidal Deformability (array): The array that contains correpsonding Tidal property, These are dimension-less.

Return type:

Mass (array)

TOVsolver.solver_code.tidal_deformability(y2, Mns, Rns)[source]

Compute Tidal deformability from y2, neutron star mass and raius

Parameters:

  • y2 (array) – midiate varrible that computing tidal

  • Mns (array) – neutron star mass in g/cm3

  • Rns (array) – neutron star radius in cm.

Returns:

neutron star tidal deformability with unit-less.

Return type:

tidal_def (array)