Figure 4

Figure 4: Isodensity contours and velocity profile in the equatorial plane for a merger of two equal-mass NSs with MNS = 1.5M ⊙ assumed to follow the APR model [3] for the NS EOS. With a higher mass than the remnant shown in Figure 3, the remnant depicted here collapses promptly to form a BH, its horizon shown by the dashed blue circle, absorbing all but 0.004% of the total rest mass from the original system. Image reproduced by permission from Figure 5 of [144], copyright by APS.