From 32d6a80f96c4dee9164abefdb478b37eb1a342bb Mon Sep 17 00:00:00 2001 From: Eric Teunis de Boone Date: Tue, 14 Nov 2023 12:23:16 +0100 Subject: [PATCH] Thesis: Introduction: Random Writes --- documents/thesis/chapters/introduction.tex | 11 ++++++----- 1 file changed, 6 insertions(+), 5 deletions(-) diff --git a/documents/thesis/chapters/introduction.tex b/documents/thesis/chapters/introduction.tex index 3883707..b8c8ae9 100644 --- a/documents/thesis/chapters/introduction.tex +++ b/documents/thesis/chapters/introduction.tex @@ -8,7 +8,7 @@ } \begin{document} -\chapter{Introduction} +\chapter{Cosmic Rays and Extensive Air Showers} \label{sec:introduction} %<<< % Intro Cosmic Ray @@ -20,7 +20,7 @@ With many discoveries following, the field of (astro-)particle physics evolved. Large collaborations are now detecting cosmic rays with a variety of methods over a large range of energy (see Figure~\ref{fig:cr_flux}). \\ % Radio -In the last decade, the detection using radio antennas has received significant attention \Todo{ref}, such that collaborations such as the~\gls{GRAND}\Todo{more?} are building observatoria that fully rely on radio measurements. +In the last two decades, the detection using radio antennas has received significant attention \Todo{ref}, such that collaborations such as the~\gls{GRAND}\Todo{more?} are building observatoria that fully rely on radio measurements. % For such radio arrays, the analyses require an accurate timing of signals within the array. Generally, \glspl{GNSS} are used to synchronise the detectors. @@ -68,9 +68,10 @@ Unfortunately, this weak interaction also troubles the detection of the neutrino \includegraphics[width=\textwidth]{astroparticle/The_CR_spectrum_2023.pdf} \caption{ From \protect \cite{The_CR_spectrum}. - The diffuse cosmic ray spectrum as measured by various experiments. + The diffuse cosmic ray spectrum (upper line) as measured by various experiments. The intensity and fluxes can generally be described by rapidly decreasing power laws. - The grey shading indicates the order of magnitude of the particle flux, such that from the ankle onwards ($E>10^9\GeV$) the flux reaches $1/km^2/yr$. + The grey shading indicates the order of magnitude of the particle flux, such that from the ankle onwards ($E>10^9\GeV$) the flux reaches $1$~particle per~square~kilometer per~year. + \protect \Todo{Knee - (inter)galactic} } \label{fig:cr_flux} \end{figure}%>>> @@ -79,7 +80,7 @@ Unfortunately, this weak interaction also troubles the detection of the neutrino % Energy Cosmic rays span a large range of energy and flux as illustrated in Figure~\ref{fig:cr_flux}. At lower energies, the flux is high enough for direct detection. -At energies above $10^{6}\GeV$, the flux decrease requires indirect detection methods. +At energies above $10^{6}\GeV$, however, the flux decrease requires indirect detection to obtain decent statistics. \\ % Acceleration The acceleration of high energy cosmic rays is thought to occur in highly energetic regions.