some more refinements

Physics_Thesis_Template/content/chapter-discussion.tex

@@ -16,7 +16,7 @@ Limiting the flare by maximum flare peak height indicates a dependency of flares
 %Limit to max 1.05, nearly identical histograms to all data. (different result to \cite{connection_starspots_flares_ms_kepler})
 %\\\\
 
-Out of a total of \textasciitilde40 K dwarfs in the list of stars to be analyzed, flares could only be detected on 37 stars. This could be due to a not sensitive enough algorithm or instruments, too noisy data or it could be that there were just no flares during the observation time. Overall the results for the flare distribution on K dwarfs is similar to those of M dwarfs. There is no real dependence on spots visible, with the exception of the bin (bins for the histogram with 30 bins) around the phase minimum. One of the causes for this is V* V471 Tau (see section \ref{results:v471_tau}), which is in close orbit with a white dwarf (\cite{v471tau_revised}, \cite{V471tau_magnetic_activity}). This can lead to magnetic interactions between the K dwarf and the white dwarf (\cite{V471tau_magnetic_activity}), which could lead to the increased flarecount seen.\\
+Out of a total of \textasciitilde40 K dwarfs in the list of stars to be analyzed, flares could only be detected on 37 stars. This could be due to a not sensitive enough algorithm or instruments, too noisy data or it could be that there were just no flares during the observation time. Overall the results for the flare distribution on K dwarfs is similar to those of M dwarfs. With the exception of the bin (bins for the histogram with 30 bins) around the phase minimum. This bin shows a significantly increased flare count. One of the, but not the sole cause for this is V* V471 Tau (see section \ref{results:v471_tau}), which is in close orbit with a white dwarf (\cite{v471tau_revised}, \cite{V471tau_magnetic_activity}). This can lead to magnetic interactions between the K dwarf and the white dwarf (\cite{V471tau_magnetic_activity}), which could lead to the increased flarecount seen.\\
 Limiting the flare peaks to greater than 5\% of the flux shows two peaks around the center bin, with one higher bin being at the maximum at phase $0 \pi$. While the two peaks around the phase minimum could indicate a dependency on spots, it is not the only relevant bin found.
 Limiting the flare peaks to a maximum of 1\% above the flux shows an interesting pattern. There is a larger count of flares found during the phase minimum, but also during the phase maximum, while less flares have been detected in the transition between phase miminum/maximum. Increasing the allowed flare peak to 5\% above the flux shows a similar pattern, but the gaps between peaks/dips closes and is already very similar to the histogram with all flares.
 
@@ -36,7 +36,7 @@ Out of a total of \textasciitilde13 F dwarfs in the list of stars to be analyzed
 
 % For F dwarfs, overall too little data, but the not siginificant amount detected all during phase minimum, could be similar to G dwarfs?
 
-Looking at all results together, there appears to be a slight flare dependence, which is mostly influenced by the results for K and G stars. The dip in the otherwise seemingly stable histogram for the results of M dwarfs propagates for the overall results. 
+Looking at all results together, there appears to be a slight flare dependence, which is mostly influenced by the results for K and G stars. The dip in the otherwise seemingly stable histogram for the results of M dwarfs propagates for the overall results. All results will be published on github. The program will be available at \href{URL}{text} while the data will be available at \href{URL}{text}.
 
 % All data combined, peak at phase minimum dominated by G/K dwarfs, dip in transition maxima -> minima dominated by dip from M dwarf results.