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Figure 1:
The three applications of characteristic evolution with data given on an initial null hypersurface N and boundary B. The shaded regions indicate the corresponding domains of dependence. |
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Figure 2:
The null parallelogram. After computing the field at point ![]() ![]() ![]() ![]() ![]() ![]() |
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Figure 3:
Trousers shaped event horizon obtained by the conformal model. |
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Figure 4:
Upper left: Tidal distortion of approaching black holes Upper right: Formation of sharp pincers just prior to merger. Middle left: Temporarily toroidal stage just after merger. Middle right: Peanut shaped black hole after the hole in the torus closes. Lower: Approach to final equilibrium. |
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Figure 5:
The physical setup for the scattering problem. A star of mass ![]() ![]() ![]() ![]() ![]() ![]() ![]() |
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Figure 6:
Black hole excision by matching. A Cauchy evolution, with data at ![]() ![]() ![]() ![]() ![]() ![]() ![]() |
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Figure 7:
Sequence of slices of the metric component ![]() |
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Figure 8:
CCM for binary black holes, portrayed in a co-rotating frame. The Cauchy evolution is matched across two inner worldtubes ![]() ![]() ![]() ![]() |
http://www.livingreviews.org/lrr-2012-2 |
Living Rev. Relativity 15, (2012), 2
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