We present a study of the merger of six different known galactic systems of
binary neutron stars (BNS) of unequal mass with a mass ratio between 0.75 and
0.99. Specifically, these systems are J1756-2251, J0737-3039A, J1906+0746,
B1534+12, J0453+1559 and B1913+16. We follow the dynamics of the merger from
the late stage of the inspiral process up to ∼ 20 ms after the system has
merged, either to form a hyper-massive neutron star (NS) or a rotating black
hole (BH), using a semi-realistic equation of state (EOS), namely the
seven-segment piece-wise polytropic SLy with a thermal component. For the most
extreme of these systems (q=0.75, J0453+1559), we also investigate the
effects of different EOSs: APR4, H4, and MS1. Our numerical simulations are
performed using only publicly available open source code such as, the Einstein
Toolkit code deployed for the dynamical evolution and the LORENE code for the
generation of the initial models. We show results on the gravitational wave
signals, spectrogram and frequencies of the BNS after the merger and the BH
properties in the two cases in which the system collapse within the simulated
time.Comment: 13 pages, 10 figure
