Microscopic Black Holes and Cosmic Shells

TL;DR

This thesis investigates microscopic black holes' radiation spectra, including gamma rays and neutrinos, and explores scalar field solutions with shell structures in a de Sitter universe, combining astrophysics and gravitational theory.

Contribution

It provides detailed numerical solutions for black hole outflows and radiation spectra, and demonstrates the existence of scalar field shell solutions in a de Sitter spacetime.

Findings

Calculated gamma ray and neutrino spectra from black holes.

Identified shell-type solutions of scalar fields with no singularities.

Suggested observational signatures for microscopic black holes.

Abstract

In the first part of this thesis the relativistic viscous fluid equations describing the outflow of high temperature matter created via Hawking radiation from microscopic black holes are solved numerically for a realistic equation of state. We focus on black holes with initial temperatures greater than 100 GeV and lifetimes less than 6 days. The spectra of direct photons and photons from neutral pion decay are calculated for energies greater than 1 GeV. We calculate the diffuse gamma ray spectrum from black holes distributed in our galactic halo. However, the most promising route for their observation is to search for point sources emitting gamma rays of ever-increasing energy. We also calculate the spectra of all three flavors of neutrinos arising from direct emission from the fluid at the neutrino-sphere and from the decay of pions and muons from their decoupling at much larger radii and smaller temperatures for neutrino energies between 1 GeV and the Planck energy. The results for neutrino spectra may be applicable for the last few hours and minutes of the lifetime of a microscopic black hole. In the second part of this thesis the combined field equations of gravity and a scalar field are studied. When a potential for a scalar field has two local minima there arise spherical shell-type solutions of the classical field equations due to gravitational attraction. We establish such solutions numerically in a space which is asymptotically de Sitter. It generically arises when the energy scale characterizing the scalar field potential is much less than the Planck scale. It is shown that the mirror image of the shell appears in the other half of the Penrose diagram. The configuration is smooth everywhere with no physical singularity.