Neutron-Star – Black-Hole Coalescence

Neutron-Star – Black-Hole Coalescence

with tidal disruption

The images show a simulation of a neutron-star–black-hole coalescence in which the neutron star is tidally disrupted during the merger.
In general, tidal disruption is present for low-mass black holes, prograde black hole spins, or large neutron star radii. However, such scenarios seem less present in nature, e.g., the neutron-star–black-hole coalescences GW200105 and GW200115 showed both no sign of tidal disruption.

Numerical relativity simulation: S.V. Chaurasia (Stockholm University), T. Dietrich (Potsdam University and Max Planck Institute for Gravitational Physics)
Scientific visualization: T. Dietrich (Potsdam University and Max Planck Institute for Gravitational Physics), N. Fischer, S. Ossokine, H. Pfeiffer (Max Planck Institute for Gravitational Physics), T. Vu

We acknowledge support through the High-Performance Computing Center Stuttgart (HLRS) through project GWanalysis (project 44189) for HAWK, through the Norddeutsche Verbund für Hoch- und Höchstleistungsrechnen (project bbp00049), and through the PDC Center for High Performance Computing (SNIC 2020/1-34) for Beskow. This support enables our simulations of black hole - neutron star systems.

Note: Publication of these images and movies requires proper credits and written permission. Please contact the in advance of publication or for higher-resolution versions.

Fig. 1
Fig. 2
Go to Editor View