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Thesis: Introduction: Random Writes

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documents/thesis/chapters/introduction.tex
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@ -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.