The problem of detecting gravitational radiation is receiving considerable attention with the construction of new detectors in the United States, Europe, and Japan. The theoretical modeling of the wave forms that would be produced in particular systems will expedite the search for and analysis of detected signals. The characteristic formulation of GR is implemented to obtain an algorithm capable of evolving black holes in 3D asymptotically flat spacetimes. Using compactification techniques, future null infinity is included in the evolved region, which enables the unambiguous calculation of the radiation produced by some compact source. A module to calculate the waveforms is constructed and included in the evolution algorithm. This code is shown to be second-order convergent and to handle highly non-linear spacetimes. In particular, we have shown that the code can handle spacetimes whose radiation is equivalent to a galaxy converting its whole mass into gravitational radiation in one second. We further use the characteristic formulation to treat the region close to the singularity in black hole spacetimes. The code carefully excises a region surrounding the singularity and accurately evolves generic black hole spacetimes with apparently unlimited stability.
The second way that curves can add interest to an image is a bit more intangible. With this use of curves, the curves do not point at the center of interest. In fact, they do not point at anything in particular. Instead, the curves simply flow through the image in a graceful or dynamic way. How does this help the image? Even though the curves do not point toward any object, they still serve to control the viewer's eyes. When used properly, the viewer's eyes will roam back and forth along the curves. Thus, the viewer's attention has been captured.