We present new (3+ 1) D numerical relativity simulations of the binary neutron star (BNS)
merger and postmerger phase. We focus on a previously inaccessible region of the binary …

Matter in neutron star collisions reaches densities up to few times the nuclear saturation
threshold, \rho_0 ρ 0 and temperatures up to one hundred MeV. Understanding the structure …

The data analysis of the gravitational wave signals emitted by coalescing neutron star
binaries requires the availability of an accurate analytical representation of the dynamics …

Numerical relativity simulations of compact binaries with the Z4c and Baumgarte-Shapiro-
Shibata-Nakamura-Oohara-Kojima (BSSNOK) formulations are compared. The Z4c …

The nuclear symmetry energy plays a key role in determining the equation of state of dense,
neutron-rich matter, which governs the properties of both terrestrial nuclear matter as well as …

We study equal-and unequal-mass neutron star mergers by means of new numerical
relativity simulations in which the general relativistic hydrodynamics solver employs an …

We present a new numerical relativity code designed for simulations of compact binaries
involving matter. The code is an upgrade of the bam code to include general relativistic …

Gravitational wave (GW) detections of binary neutron star inspirals will be crucial for
constraining the dense matter equation of state (EOS). We demonstrate a new degeneracy …

Binary neutron star mergers are studied using nonlinear 3+ 1 numerical relativity simulations
and the analytical effective-one-body model. The effective-one-body model predicts …

Information about the last stages of a binary neutron star inspiral and the final merger can be
extracted from quasiequilibrium configurations and dynamical evolutions. In this article, we …