In this talk, the geometric framework of local metric deformations will be discussed with special emphasis on so‐called generalized Kerr‐Schild deformations. The consideration of precisely these deformations is justified by the fact that they lead to a comparably simple structure of Einstein's field equations, which is demonstrated using the spincoefficient formalism of Newman and Penrose. Based on the results obtained, it is shown how the field of a gravitational shockwave generated by a massless point‐like particle can be calculated at the event horizon of the stationary Kerr‐Newman black hole, while specific physical properties of the corresponding class of geometries are discussed in passing.
Albert Huber (Vienna): Gravitational Shock Waves in stationary Black Hole Spacetimes
