Substituting the momentum-velocity relation (86) into the spatial components of Equation (110), we obtain the general form of equations of motion for star ,[46, 108, 152], we have to make another choice for (see  and Appendix B.1). At 3 PN order, yet another choice of the value of the dipole moment shall be examined (see Sections 7 and 8.2).
In Equation (111), rather than the mass of star appears. Hence we have to derive a relation between the mass and . We shall derive that relation by solving the temporal component of the evolution equations (110) functionally.
Then, since all the equations are expressed with surface integrals except to be specified, we can derive the equations of motion for a strongly self-gravitating star using the post-Newtonian approximation.
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