Figure 4: Isodensity contours and velocity profile in the equatorial plane for a merger of two
equal-mass NSs with 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.
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