Black holes in tidal environments

          @misc{ scivideos_PIRSA:06110022,
            doi = {10.48660/06110022},
            url = {https://pirsa.org/06110022},
            author = {Poisson, Eric},
            keywords = {},
            language = {en},
            title = {Black holes in tidal environments},
            publisher = {Perimeter Institute for Theoretical Physics},
            year = {2006},
            month = {nov},
            note = {PIRSA:06110022 see, \url{https://scivideos.org/pirsa/06110022}}
          }
          

Abstract

A nonrotating black hole placed in a tidal environment (that is, subjected to the gravitational interactions produced by other nearby bodies) is not described by the Schwarzschild solution to the Einstein field equations. Instead, its metric is given by a perturbed version of this exact solution, and the spacetime is no longer stationary nor spherically symmetric. After reviewing the situation in Newtonian theory, I shall describe how the metric of a tidally distorted black hole is calculated. Special attention will be placed on the general description of the tidal environment, the choice of a good coordinate system to describe the perturbed black hole, and the consequences on the structure of the event horizon