some more refinements

Physics_Thesis_Template/content/chapter-results.tex

@@ -116,7 +116,7 @@ The difference becomes less obvious when increasing the bin size 30 (figure \ref
 \section{K dwarfs \label{sec:results:k_dwarfs}}
 
 This section shows the results for 37 K dwarfs for which flares could be detected. A full list of the stars used can be found in table \ref{apA:list_of_k_stars}.\\
-Figure \ref{fig:K-Flarecount-10_Bins} shows the amount of flares per phase with 10 bins of 37 K type dwarfs in used in this study. Overall the distribution is even within error, with a slight increase in flares when going from the maximum to the minimum of the lightcurve at phase $0.5 \pi$, and a slight decrease when going from minimum to maximum at phase $1.5 \pi$. There is also a peak at around $1 \pi$ with around 95 flares compared to the 60-80 flares per bin in the rest of the histogram. This peak is dominated by $V*~V471~Tau$. The individual results for this star are visible in section \ref{sec:results:individual}.\\
+Figure \ref{fig:K-Flarecount-10_Bins} shows the amount of flares per phase with 10 bins of 37 K type dwarfs in used in this study. Overall the distribution is even within error, with a slight increase in flares when going from the maximum to the minimum of the lightcurve at phase $0.5 \pi$, and a slight decrease when going from minimum to maximum at phase $1.5 \pi$. There is also a peak at around $1 \pi$ with around 95 flares compared to the 60-80 flares per bin in the rest of the histogram. One of the major contributions is V* V471 Tau. The individual results for this star are visible in section \ref{sec:results:individual}.\\
 Looking at the same dataset with 30 bins for the histogram (figure \ref{fig:K-Flarecount-30_Bins}), the peak in the phase minimum at $1 \pi$ is still visible. Additionally there appear more peaks at phase $>1.3 \pi$ ($1.3,~1.6,~1.9 \pi$), while the amount of flares between phase $0 \pi$ and $1 \pi$ shows a slight trend to more flares with dips inbetween and a larger dip right before and after the big peak at phase $1 \pi$ which was also visible in figure \ref{fig:K-Flarecount-10_Bins} with 10 bins. The major dips at phase $0.7 \pi$, $1.3 \pi$, $1.6 \pi$ and $1.9 \pi$ are all well outside the errorbars of the surrounding peak bins, while the smaller ones between phase $0 \pi$ and $1 \pi$ overlap with their errorbars with their surrounding bins.
 
 \begin{figure}[pt!]
@@ -498,7 +498,7 @@ Increasing the bins to 30 (figure \ref{fig:V471Tau-Flarecount-30_Bins}) does not
     \label{fig:V471Tau-Flarecount}
 \end{figure}
 
-Looking at the folded lightcurves for this star (see figures \ref{fig:V471Tau-TESS42_foldedLC}, \ref{fig:V471Tau-TESS43_foldedLC} and \ref{fig:V471Tau-TESS44_foldedLC}), the transit of the white dwarf (sudden dip in the folded lightcurve) is clearly visible, and always happens around phase 0.
+Looking at the folded lightcurves for this star (see figures \ref{fig:V471Tau-TESS42_foldedLC}, \ref{fig:V471Tau-TESS43_foldedLC} and \ref{fig:V471Tau-TESS44_foldedLC}), the transit of the white dwarf (sudden dip in the folded lightcurve) is clearly visible, and always happens around phase 0. Additional folded lightcurves can be seen in appendix \ref{apB:V471_tau}, figure \ref{apB:fig:V471Tau-TESS_foldedLC} like the ones which were folded by the rotational period for when a spot modulation was detected.
 
 \begin{figure}[pt!]
     \centering