With the recent advent of multi-messenger gravitational-wave astronomy and in anticipation of more sensitive , next-generation gravitational-wave detectors , we investigate the dynamics , gravitational-wave emission , and nucleosynthetic yields of numerous eccentric binary neutron-star mergers having different equations of state .
For each equation of state we vary the orbital properties around the threshold of immediate merger , as well as the binary mass ratio .
In addition to a study of the gravitational-wave emission including f -mode oscillations before and after merger , we couple the dynamical ejecta output from the simulations to the nuclear-reaction network code SkyNet to compute nucleosynthetic yields and compare to the corresponding results in the case of a quasi-circular merger .
We find that the amount and velocity of dynamically ejected material is always much larger than in the quasi-circular case , reaching maximal values of M _ { ej,max } \sim 0.1 M _ { \odot } and v _ { max } / c \sim 0.75 .
At the same time , the properties of this material are rather insensitive to the details of the orbit , such as pericenter distance or post-encounter apoastron distance .
Furthermore , while the composition of the ejected matter depends on the orbital parameters and on the equation of state , the relative nucleosynthetic yields do not , thus indicating that kilonova signatures could provide information on the orbital properties of dynamically captured neutron-star binaries .