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Back to Basics...in 3-D

Single, non-rotating black hole

All the movies so far have shown axisymmetric spacetimes. i.e., all the spacetimes had a rotation symmetry about some axis, making the problem effectively 2D. In order to solve the most general 2 black hole collision problem, we will have to lift any symmetry requirements, and do full 3D simulations.

This movie shows data from a full 3D code. Although this simulation was done using 3D Cartesian coordinates, the problem being solved is a spherically symmetric black hole. This problem was chosen as the first black hole test problem of the 3D code, because it is the simplest spacetime containing a black hole. Also, we know what answers to expect because of extensive tests done with 1D codes.

This movie shows the time development of the "radial metric function grr" that measures the distance between points in the radial direction out from the center of the black hole. The height of the graph represents the value of grr, which is plotted for the x-y plane (z=0). Only one quadrant (x>0 and y>0) is shown in the movie. The function develops a large, spherical peak surrounding the black hole, which is expected from earlier 1D studies. This simulation was run until about t=30M, where M is the mass of the black hole, and then the movie loops backward to the initial time, t=0.

Research Paper on three dimensional numerical relativity.


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Copyright, (c) 1995: Board of Trustees, University of Illinois


NCSA. Last modified 11/9/95.