Video URL

https://pirsa.org/24010086

Reflecting boundary conditions in numerical relativity as a model for black hole echoes

Dailey, C. (2024). Reflecting boundary conditions in numerical relativity as a model for black hole echoes. Perimeter Institute for Theoretical Physics. https://pirsa.org/24010086

Dailey, Conner. Reflecting boundary conditions in numerical relativity as a model for black hole echoes. Perimeter Institute for Theoretical Physics, Jan. 22, 2024, https://pirsa.org/24010086 

          @misc{ scivideos_PIRSA:24010086,
            doi = {10.48660/24010086},
            url = {https://pirsa.org/24010086},
            author = {Dailey, Conner},
            keywords = {Other Physics},
            language = {en},
            title = {Reflecting boundary conditions in numerical  relativity as a model for black hole echoes},
            publisher = {Perimeter Institute for Theoretical Physics},
            year = {2024},
            month = {jan},
            note = {PIRSA:24010086 see, \url{https://scivideos.org/pirsa/24010086}}
          }

Conner Dailey Perimeter Institute for Theoretical Physics

DOI 10.48660/24010086
Source Repository PIRSA
Collection
Talk Type Scientific Series
Subject

Abstract

Recently, there has been much interest in black hole echoes, based on the idea that there may be some mechanism (e.g., from quantum gravity) that waves/fields falling into a black hole could partially reflect off of an interface before reaching the horizon. There does not seem to be a good understanding of how to properly model a reflecting surface in numerical relativity, as the vast majority of the literature avoids the implementation of artificial boundaries, or applies transmitting boundary conditions. Here, we present a framework for reflecting a scalar field in a fully dynamical spherically symmetric spacetime, and implement it numerically. We study the evolution of a wave packet in this situation and its numerical convergence, including when the location of a reflecting boundary is very close to the horizon of a black hole. This opens the door to model exotic near-horizon physics within full numerical relativity.