Causal Structure and Horizon Stability of Black Holes in Curved Spacetimes

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Abstract/Contents

Abstract
The causal structure of spacetime encodes basic information about how different events influence each other, allowing us to better understand our universe. In this thesis, we study the causal structure of Schwarzschild and Reissner–Nordström (RN) black holes in de Sitter (dS) and Anti-de Sitter (AdS) spacetimes. We find that the inner horizon of RN black holes is highly unstable and analyze how its conformal diagram evolves from the Schwarzschild conformal diagram. We illustrate the Penrose diagrams for uncharged and charged black holes within the constant curvature spacetimes and analyze their properties. We examine the smallest black holes in dS, finding their probability of nucleation, as well as the largest dS black holes, which lead to the Nariai solution. We demonstrate two methods for finding the Nariai geometry of RNdS, with the caveat that the inner horizon remains highly unstable. Finally, we find a parallel between gravitational and matrix methods, confirming that the underlying holographic description of dS relies on matrix quantum mechanics.

Description

Type of resource text
Date modified December 5, 2022
Publication date June 10, 2022; May 2022

Creators/Contributors

Author Tabor, Elisa
Thesis advisor Susskind, Leonard
Thesis advisor Stanford, Douglas
Degree granting institution Stanford University
Department Department of Physics

Subjects

Subject de Sitter
Genre Text
Genre Thesis

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Preferred citation
Tabor, E. (2022). Causal Structure and Horizon Stability of Black Holes in Curved Spacetimes. Stanford Digital Repository. Available at https://purl.stanford.edu/mh237tg6127

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Undergraduate Theses, Department of Physics

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