**General Relativity**

I began my scientific career in 1970, just two years after the term “black hole” was coined. This early entry into the rapidly developing field enabled me to discover what is now termed the Smarr Mass Formula for black holes. I was also the first to determine the intrinsic curvature deformation caused by rotation in black holes. Although the numerical solution of strong-field perturbation theory of spherical and rotating black holes had been well developed, the solution of the Cauchy evolution by computational solution of partial differential equations required a number of Riemannian geometry innovations that my co-workers and I developed. At Harvard, I was able to work with their elementary particle group to compare field theoretic behavior of spin 1 and spin 2 (gravity) for self-attracting solutions, as well as help develop new spacecraft tests for general relativity.

Working under the mentorship of general relativity and quantum gravity pioneer Bryce DeWitt, I helped found the field of numerical relativity by amalgamating techniques from differential geometry, general relativity, numerical analysis, and computer graphics and applying them to the two-body problem in general relativity in the form of the head-on collision of two black holes. This led to the first computation of the gravitational radiation from colliding black holes, which was observed 40 years later in 2015. With my students and colleagues I also computationally investigated black hole dynamics, gravitational collapse, and black hole/gravitational wave interactions.