Geometry of Black Hole Spacetimes

doi:10.1017/9781108186612.002

2 - Geometry of Black Hole Spacetimes

Published online by Cambridge University Press: 21 December 2017

Lars Andersson ,

Thomas Bäckdahl and

Pieter Blue

Edited by

Thierry Daudé ,

Dietrich Häfner and

Jean-Philippe Nicolas

Show author details

Lars Andersson: Affiliation:
Albert Einstein Institute
Thomas Bäckdahl: Affiliation:
Chalmers University of Technology
Pieter Blue: Affiliation:
University of Edinburgh
Thierry Daudé: Affiliation:
Université de Cergy-Pontoise
Dietrich Häfner: Affiliation:
Université Grenoble Alpes
Jean-Philippe Nicolas: Affiliation:
Université de Bretagne Occidentale

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Summary

Abstract. These notes, based on lectures given at the summer school on Asymptotic Analysis in General Relativity, collect material on the Einstein equations, the geometry of black hole spacetimes, and the analysis of fields on black hole backgrounds. The Kerr model of a rotating black hole in a vacuum is expected to be unique and stable. The problem of proving these fundamental facts provides the background for the material presented in these notes.

Among the many topics which are relevant to the uniqueness and stability problems are the theory of fields on black hole spacetimes, in particular for gravitational perturbations of the Kerr black hole and, more generally, the study of nonlinear field equations in the presence of trapping. The study of these questions requires tools from several different fields, including Lorentzian geometry, hyperbolic differential equations, and spin geometry, which are all relevant to the black hole stability problem.

Introduction

A short time after Einstein published his field equations for general relativity in 1915, Karl Schwarzschild discovered an exact and explicit solution of the Einstein vacuum equations describing the gravitational field of a spherical body at rest. In analyzing Schwarzschild's solution, one finds that if the central body is sufficiently concentrated, light emitted from its surface cannot reach an observer at infinity. It was not until the 1950s that the global structure of the Schwarzschild spacetime was understood. By this time causality theory and the Cauchy problem for the Einstein equations were firmly established, although many important problems remained open. Observations of highly energetic phenomena occurring within small spacetime regions, eg. quasars, made it plausible that black holes played a significant role in astrophysics, and by the late 1960s these objects were part of mainstream astronomy. The term “black hole” for this type of object came into use in the 1960s. According to our current understanding, black holes are ubiquitous in the universe, in particular most galaxies have a supermassive black hole at their center, and these play an important role in the life of the galaxy.

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Type: Chapter
Information: Asymptotic Analysis in General Relativity , pp. 9 - 85

DOI: https://doi.org/10.1017/9781108186612.002 [Opens in a new window]

Publisher: Cambridge University Press

Print publication year: 2018

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