General Relativistic Eccentric Binary Neutron Star Merger

This is a simulation of binary neutron star on highly eccentric orbit done in full general relativity (See article for more details). We analyze the f-mode oscillations induced during close encounters before the merger of the two stars. The energy stored in these oscillations can be as large as 10^{-3}Msun ~ 10^{51} erg (energy in a supernova!).

Gravitational waves from GW170817

Simulations dedicated to follow up on GW170817; the first combined detection of gravitational waves, a gamma ray burst, and a kilonova, please visit the AEI homepage for additional material.

Gravitational waves during the merger of PSR J0737-3039

Simulation of the double pulsar system PSR J0737-3039, anticipating the emitted gravitational wave signal in more than 50 million years when the two stars will finally merge.

High mass ratio mergers

Animation showing a merger of two neutron stars with a mass ratio of q=1.5.