Figure 18: Isodensity contours in the equatorial plane for the merger of a
neutron-star binary (left panel) and a case. Vectors indicate the local velocity
field . The image corresponds to the final snapshot of the evolution for the two models.
The outcome of the merger for the more massive case is the delayed formation of a black hole, as
signalled by the collapse of the lapse function shown in the lower panel of the image. In the less
massive case, a long-lived hypermassive neutron star supported by rotation is formed. Simulations
performed by [372]. (Used with permission.)
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