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)

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)

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, energy_density, pressure)

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.

Return type:

Mass (array)

TOVsolver.solver_code.solveTOV_tidal(center_rho, energy_density, pressure)

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)

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)