Status: Published 16 February 2024. Phys.Rev.D 109, 044033. Based on arXiv:2109.01193.
Tidal deformation of dynamical horizons in binary black hole mergers and its imprint on gravitational radiation
Vaishak Prasad.
Resources:
The draft is on [arXiv].
Overleaf repository:
To be updated soon.
qlmtools : Functions to handle 2D dynamical horizon data.
Media
The above movie shows the quasi-circular inspiral of two non-spinning black holes of mass ratio 0.6 and the tidal deformations of black hole horizons in the due course of the merger. This mass-ratio is very close to that of GW190521, however the black
holes are non-spinning in this simulation. The deformation of the dynamical horizons of the black holes can be directly quantified and visualized in terms of the intrinsic curvature of the two-dimensional slices of the dynamical horizon. The values of the 2D Ricci scalar are shown on the color bars. This movie shows that the deformation of the horizon geometry is mutual for both the horizons and the Ricci scalar distribution patterns face each other at all points on the orbit. It can be seen that, like for the gravitational waves received at null infinity from such a system, the quadrupolar component is the dominant contribution to the horizon multipole moment. On the bottom, the dominant (2,2) mode of the gravitational radiation emitted from the system recorded in a detector placed at 100M units from its center is shown. Approximately, 17 cycles of the dominant gravitational waveform mode are emitted before the merger happens i.e. the black holes travel on around 8.5 complete orbits. This movie was made using numerical relativity simulation of binary black holes using the high-performance computing cluster Pegasus at IUCAA. The EinsteinToolkit was used to carry out the simulations and VisIt was used in making the movie. See [1], [2] for further details.
[1] Generalized multipole moments of dynamical horizons in binary black hole mergers
[2] Tidal deformation of dynamical horizons in binary black hole mergers