### 4.6 Newtonian equations of motion

We first derive the Newtonian equations of motion and the 1 PN correction to the acceleration. The
derivation of the 1 PN equations of motion includes some essences of our formalism and shows how it works
properly. Thus we shall give a detailed explanation about the derivation, though the calculation is
elementary and the resulting equations of motion are well-known.
Now let us derive the Newtonian mass-energy relation first. From Equations (102, 103) and the time
component of Equation (110), we have

Then we define the mass of star as the integrating constant of this equation,
here is the ADM mass that star had if it were isolated. (We took zero limit in
Equation (114) to ensure that the mass defined above does not include the effect of the companion star and
the orbital motion of the star itself. By this limit we ensure that this mass is the integrating constant
of Equation (113).) By definition is constant. Then we obtain the lowest order :
Second, from Equation (91) with Equations (102) and (103) we obtain at the lowest order.
Thus we have the Newtonian momentum-velocity relation from Equation (86) (we
set ).

Substituting Equation (104) with the lowest order into the general form of equations
of motion (111) and using the Newtonian momentum-velocity relation, we have for star :

where is the integral variable and . We defined as the spatial unit
vector
emanating from , , and . We used and .
For details see Figure 3).
In the above equation, by virtue of the angular integral the first term (which is singular when the
zero limit is taken) vanishes. The third term vanishes by letting go to zero. Only the second term
survives and gives the Newtonian equations of motion as expected. This completes the Newtonian order
calculations.