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Thesis: spell-check

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Eric-Teunis de Boone 2023-11-17 15:07:19 +01:00
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documents/thesis/chapters/introduction.tex
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@ -40,7 +40,7 @@ It is therefore only at the very highest energies that the direction of an initi
% CR: galaxy / extra-galactic
The same argument (but in reverse) can be used to explain the steeper slope from the ``knee'' ($10^{6}\GeV$) onwards in Figure~\ref{fig:cr_flux}.
The acceleration of cosmic rays equally requires strong and sizable magnetic fields.
The acceleration of cosmic rays equally requires strong and sizeable magnetic fields.
Size constraints on the Milky~Way lead to a maximum energy for which a cosmic ray can still be contained in our galaxy.
It is thus at these energies that we can distinguish between galactic and extra-galactic origins.
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@ -67,7 +67,7 @@ Figure~\ref{fig:airshower:depth} shows the number of particles as a function of
The atmospheric depth at which this number of particles reaches its maximum is called $\Xmax$.
\pagebreak
In Figure~\ref{fig:airshower:depth}, $\Xmax$ is different for the airshowers generated by a photon, a proton or an iron nucleus.
In Figure~\ref{fig:airshower:depth}, $\Xmax$ is different for the air showers generated by a photon, a proton or an iron nucleus.
Typically, heavy nuclei have their first interaction higher up in the atmosphere than protons, with photons penetrating the atmosphere even further.
Therefore, accurate measurements of $\Xmax$ allow to statistically discriminate between photons, protons and iron nuclei.
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