- #1

BiGyElLoWhAt

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So the time-time should be approximately E/c^2V, so for the earth moon system

##T_{00} = \frac{3}{4\pi r_E^3}\frac{1}{c^2}(M_Ec^2 + 2/5 M_Er_E^2\omega^2)##

from 0 to r_E + [same for the moon] but from [center of the moon as a function of time] to [radius of the moon]

I guess my question is how do I rigorously add in these limits? So if I wanted to include the earth, sun, and moon, these limits on the location of the energy density/c^2 will be more noticeably important.

Certainly I don't have to write it as a fourier or taylor series, right? Right?

Any help is appreciated.