Speaker
Gabriele Travaglini
Description
We will discuss the computation of classical tree-level five-point scattering amplitudes for the two-to-two scattering of spinning celestial objects with the emission of a graviton. Using this result, we will 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.
| I read the instructions above | Yes |
|---|
