Figure 3

Figure 3: Isodensity contours and velocity profile in the equatorial plane for a merger of two equal-mass NSs with MNS = 1.4M ⊙ assumed to follow the APR model [3] for the NS EOS. The hypermassive merger remnant survives until the end of the numerical simulation. Image reproduced by permission from Figure 4 of [144], copyright by APS.