by eliminating the conformal time $\eta$ from , . Then, the above formula for the radiation of a precessing *neutral* object would become $$\label{eq:effectivepower}
\frac{d \cE}{dt}      =  e^2  \left(\frac{\lambda_P a(0)}{a(t)} \right)^4 M^2 R^2 \omega^6.$$ This energy has to be emitted of course at the cost of the kinetic energy of the rotating object due to spin, precession and orbital rotation, as well as of its potential energy, causing a faster inspiraling. For simplicity, we will consider here only the orbital kinetic term, and then $$\label{eq:conservation}
\frac{d}{dt}\left(\frac12M R^2 \omega^2\right) = - \frac{d \cE}{dt},$$ which entails that the total radiated energy can be estimated as $$\label{eq:totalenergy}
\cE = \frac12M R^2 \left[\omega_0^2 - \omega(t_{collapse})^2\right],$$ where the integration cannot be extended beyond the hiding of our object within the event horizon of the other. For the radiated power according to our formulae near the singularity would diverge, but would remain trapped and would not be visible from outside.

According to , the total radiated energy can be sizable only if $\omega(t_{collapse}) \ll \omega_0$. In order to check if this is the case in typical situations, we solve , that, inserting , becomes $$\dot \omega = - e^2(\lambda_P a(0))^4M \frac{\omega^5}{a(t)^4},$$ which can be integrated by 