\chapter{Conclusion and Outlook \label{sec:conclusion}}

% better algorithms, handle edge cases better, analyse more stars, take kepler/k2 long cadence into consideration for more data, create plots for flare peaks between x and y

In conclusion the only cumulative results which shows a significant spot dependence are those for G type stars. This distribution shows a significant increase in flares during the phase minimum over the overall flare distribution. The distribution shows a strong similarity to a normal distribution. The same accounts for the two selected G type stars BD-08 995 and TYC 4595-107-1 which were presented and discussed. The histograms for K dwarfs on the other hand do not reveal similarities to a normal distribution. There appears a singular peak in the histogram with 10 bins at the phase minimum, with a few additional narrower peaks in the histogram with 30 bins. This could indicate a dependence of some sort, but a more detailed view at the individual stars is needed. As this category includes V* V471 Tau (close binary system with a white dwarf), similar interactions could happen on other stars. While there is no significant result for a spot dependence of the detected flares on M dwarfs, some individual stars show a behaviour similar to G-stars. HK Aqr and KOI-256 are here good examples, whereas 2MASS J19230963+3739397 shows few flares in the minimum but more flares in the maximum of the phasefolded lightcurve.\\
Overall improvements to the folding algorithms are required to handle edge cases better (e.g. KOI-256) , while not breaking for others. This could either be done automatically, or by setting special parameters for individual stars. Even though the latter would require manual user interaction and checking the edge cases manually. Additionally a common folding epoch for multiple fits files of the same star could be implemented. A good example would be V471 Tau, which showed a consistent spot modulation in some of its TESS lightcurves which differed from its rotational period. Implementing something like this could guarantee that the (in this case) transit of the white dwarf would always be at the same position in the phase, and not "jumping" between the center and the edges. Furthermore the energy for the flares could be calculated. For this improvments for the flare duration algorithm is required though, as it currently is just an estimation and does not account for the longest flare durations. It neither makes a distinction between TESS lightcurves with a 2 minute cadence and the Kepler/K2 short cadence data which has a cadence of 1 minute.\\
Furthermore more stars could be taken into consideration. While the Kepler/K2 missions are complete, the TESS mission is being extended and still observing as of writing this thesis. One could also take into account Kepler long cadence data (30 minute cadence), which would not be able to detect shorter duration flares, but being available for a larger amount of stars.
