Resummed spinning waveforms from five-point amplitudes

Understand

We compute the classical tree-level five-point amplitude for the two-to-two scattering of spinning celestial objects with the emission of a graviton.

• Using this five-point amplitude, we then turn to the computation of the leading-order time-domain gravitational waveform.
• The method we describe is suitable for arbitrary values of classical spin of Kerr black holes and does not require any expansion in powers of the spin.
• In this paper we illustrate it in the simpler case of the scattering of one Kerr and one Schwarzschild black hole.