Solve TOV Equation

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

TOV_solver.TOV(r, y, inveos)

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)

TOV_solver.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}

• Test_EOS.csv (still please check the) –

• is (the conversion) –

• (g/cm3)*G/c**2 –

• example. (that should will convert it to here in) –

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

• MeV/fm^{-3} (with) –

• Test_EOS.csv –

• is –

• (dyn/cm3)*G/c**4. –

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)

TOV_solver.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)