\chapter{Discussion \label{sec:discussion}}



%methods: lombscargle generally finds lower periods with higher peaks (e.g. halfs of rotational period), which boxleastsquares does not always detect within the 4 highest


%M dwarfs, all data, no significant dependency of flare appearance on phase using 10 bins.
%30 bins -> either 2 dips during the transition minima <-> maxima or increase of flare occurance during minima and maxima.
%Looking at stronger flares only (min 1.25/1.5 flare peak) peaks during minima, stronger peak during phase maxima, in both 10 and 30 bin histograms.
%Limiting to max 1.01, makes dip (compared to all data) clearer. Generally more flares during maxima than minima. 
%Limit to max 1.05, nearly identical histograms to all data. (different result to \cite{connection_starspots_flares_ms_kepler})
%\\\\

% K dwarfs, all data, siginificant peak at phase minimum, peak dominated by V471 Tau (discussed later). Slightly more flares from maximum to minimum than minimum to maximum in 10 bins. 30 bins larger dips but also larger peaks in second half of phase compared to first half.
% limiting to min 1.05 -> three peaks, dip after maximum and on at phase 1 $\pi$. gradual decrease after minimum. V471 Taus peaks at right before and right after phase minimum.
% limiting to <1.01 and 1.05, makes histogram look more and more like with all data, similarly to \cite{connection_starspots_flares_ms_kepler} peak in center (compared to their M/K plot), but additionally also peak at phase maximum.
% max 1.05 already most flares, very similar to with all data.

% G dwarfs, significant results, increase of flare appearance during phase minimum. Most flares are <1.05 (flares on solar like stars that increase brightness by 0.1\% to 1\% already superflares, \cite{solar_like_superflares}) -> most/all detected flares superflares. Overall dependency on phase/spot appearance.
% Limiting to flares >1.05 -> flares during minima and transitions between minima <-> maxima, increasing bins -> more data would be required.

% For F dwarfs, overall too little data, but the not siginificant amount detected all during phase minimum, could be similar to G dwarfs?

% All data combined, peak at phase minimum dominated by G/K dwarfs, dip in transition maxima -> minima dominated by dip from M dwarf results.

% Individual star results (subset taken):
% BD-08 995 (G type): shows a strong flare/spot dependence for amount, flare peaks not dependent on phase

% TYC 1360-957-1 (K type): no clear dependence on spots for flare count (1 peak around maximum, 1 during transition, another at minimum), less siginificant with more bins
% Shows strongest flares right before phase minimum though.

% TYC 4595-107-1 (G type): similar to BD-08 995, increase of flares right before minimum, slight (less significant) increase at maximum. (appending folded lightcurves in appendix)

% V471 Tau: binary with white dwarf, most flares around white dwarf transit -> magnetic interactions likely (ref. to V471 Tau specific papers)
% Strongest flares also around that

% HK Aqr (M dwarf): not fully trusted results, half period was detected for 2/4 lightcurves (original folding had 2 fit maxima too far away from edges, caused it to check for if half period signal was detected and use that)
% only full period results show overall less flares during the maxima

% KOI-256 (M dwarf): similar issue as HK Aqr, in 2/7 Kepler, 2/3 TESS lightcurves, like V471 Tau binary with white dwarf, shows siginficant dependency on spots in with period folded results. (appending folded lightcurves in appendix)
% Largest flares, when period folded only, also at around 0.8 $\pi$ (same flare shifted to 2 $\pi$ in spot modulated fold), otherwise flare energies well spread.



