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Thesis: incorporate simple final feedback from Harm

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documents/thesis/chapters/introduction.tex
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@ -12,8 +12,6 @@
\label{sec:introduction}
%\section{Cosmic Particles}%<<<<<<
%<<<
\phantomsection
\label{sec:crs}
% Energy and flux
The Earth is bombarded with a variety of extra-terrestrial particles, with the energy of these particles extending over many orders of magnitude as depicted in Figure~\ref{fig:cr_flux}.
The flux of these particles decreases exponentially with increasing energy.
@ -57,8 +55,6 @@ Unfortunately, aside from both being much less frequent, photons can be absorbed
%>>>
%\subsection{Air Showers}%<<<
\phantomsection
\label{sec:airshowers}
When a cosmic ray with an energy above $10^{3}\GeV$ comes into contact with the atmosphere, secondary particles are generated, forming an air shower.
This air shower consists of a cascade of interactions producing more particles that subsequently undergo further interactions.
Thus, the number of particles rapidly increases further down the air shower.
@ -144,8 +140,6 @@ It is therefore important for radio detection to obtain measurements in this reg
%>>>>>>
%\subsection{Experiments}%<<<
\phantomsection
\label{sec:detectors}
As mentioned, the flux at the very highest energy is in the order of one particle per square kilometer per century (see Figure~\ref{fig:cr_flux}).
Observatories therefore have to span huge areas to gather decent statistics at these highest energies on a practical timescale.
In recent and upcoming experiments, such as the~\gls{Auger}\cite{Deligny:2023yms} and the~\gls{GRAND}\cite{GRAND:2018iaj}, the approach is typically to instrument a large area with a (sparse) grid of detectors to detect the generated air shower.