Many astrophysical high energy phenomena involve relativistic flows. We describe codes for adiabatic and isothermal flows in relativistic regimes. For adiabatic flows, we employ an equation of state (EOS) which is simple and yet approximates very closely the EOS of the single-component perfect gas. For isothermal flows, we use an EOS of constant sound speed. We present the eigenstructures of relativistic hydrodynamics which can be used to build numerical codes, and discuss the calculation of primitive variables from conservative ones for both adiabatic and isothermal flows. The shock tube tests show differences between the two flows.