Gravitational scattering of two neutron stars

We present the first numerical relativity simulations of the gravitational scattering of two neutron stars. Constraint-satisfying initial data for two equal-mass nonspinning sequences are constructed at fixed energy and various initial angular momenta (impact parameter) and evolved with Einstein equations through the scattering process. The strong-field scattering dynamics are explored up to scattering angles of 220° and the threshold of dynamical captures. The transition to bound orbits is aided by significant mass ejecta up to baryon mass <a:math xmlns:a="http://www.w3.org/1998/Math/MathML" display="inline"> <a:mrow> <a:mo>∼</a:mo> <a:mn>0.1</a:mn> <a:mrow> <a:msub> <a:mrow> <a:mi>M</a:mi> </a:mrow> <a:mrow> <a:mo stretchy="false">⊙</a:mo> </a:mrow> </a:msub> </a:mrow> </a:mrow> </a:math> . A quantitative comparison with predictions of the scattering angle from state-of-the-art effective-one-body and post-Minkowskian calculations indicates quantitative agreement for large initial angular momenta, although significant discrepancies in the tidal contribution emerge toward the capture threshold. Gravitational waveforms and radiated energy are in qualitative agreement with the analogous black hole problem and state-of-the-art effective-one-body predictions. Toward the capture threshold, waveforms from scattering dynamics carry a strong imprint of matter effects, including the stars’ <d:math xmlns:d="http://www.w3.org/1998/Math/MathML" display="inline"> <d:mi>f</d:mi> </d:math> -mode excitations during the close encounter. Overall, our simulations open a new avenue to study tidal interactions in the relativistic two-body problem.