add english abstract and update pdf

Physics_Thesis_Template/content/abstract.tex

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-\physbf{Context.~}%\lipsum[1]
+\physbf{Context.~} In recent years detection of flares and superflares on stars gained a lot of attraction, but the origin of superflares is still under debate. One possibility is that superflares are scaled up versions of normal flares, for which we would expect to find a correlation with the appearance of spots on the stars surface.
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-\physbf{Aims.~}%\lipsum[1]
+\physbf{Aims.~} This study aims to relate flares and superflares on stars to the appearance of spots on the surfaces of stars of various spectral types using Kepler/K2 and TESS lightcurves.
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 \noindent
-\physbf{Methods.~}%\lipsum[1] 
+\physbf{Methods.~} We analysed over 300 stars with a newly developed GUI application and flare detection algorithm, which can detect flares with normalized peaks of as low as 0.3\% above their surrounding flux. The lightcurves are then folded by the automatically detected spot modulation period.
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-\physbf{Results.~}%\lipsum[1]
+\physbf{Results.~} We split the results by spectral classification of the analysed stars. We also present individual results for BD-08 995, TYC 1360-957-1, TYC 4595-107-1, V* V471 Tau, V* HK Aqr, KOI-256 and 2MASS J19230963+3739397.
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-\physbf{Conclusions.~}%\lipsum[1]
+\physbf{Conclusions.~} The only cumulative results which shows a significant spot dependence are those for G type stars. The results for K type stars show one siginificant peak in the 10 bin histogram. There is not significant spot dependence for M type stars, even though some individual stars show spot dependence.
 
 
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Physics_Thesis_Template/content/chapter-introduction.tex

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 This chapter gives a brief introduction to the goals of this study, the state of the art, scientific backgrounds such as spectral types, spots and flares, as well as to the space missions from which data has been extensively used for the present study.\\
 The goal of this study is to relate flares/superflares to the appearance of spots on the surfaces of stars of various spectral types. Flares are well studied for the Sun \citep{solar_flares_1,solar_flares_2,solar_flares_3} with the first recorded event being the Carrington event from September 1859 \citep{Carrington_event}. The same accounts for the impact of stellar activity on Earths magnetic field \citep{solar_flare_mag_field}. A detailed description of spots and flares is given in section \ref{sec:intro:flares_and_spots}.
 While the first stellar flares were discovered in middle of the last century \citep{early_stellar_flares1,early_stellar_flares2}, the topic gained a lot of attraction with the launch of the likes of Kepler \citep{Kepler_first_results} and the Transiting Exoplanet Survey Satellite (TESS) \citep{TESS_release}. They allowed the survey of thousands of stars. With this, studies of flares and superflares on a large number of stars have been conducted \citep{flare_study_1,flare_study_2,connection_starspots_flares_ms_kepler,flare_occurance_periodicity}, but the origin of superflares (flares with a bolometric energy above $10^{33}$ erg) is still not clear. So far no superflare has been observed on our Sun, but there have been studies focusing on the possible origin on superflares and their likelyhood to happen on our Sun \citep{superflares_on_sun}. They found that superflares on our Sun would be rare events (every \textasciitilde800 years for superflares with $10^{34}$ erg). Even more recently \citet{superflare_shapiro} estimated the occurrence rate of superflares with $>10^{34}$ erg on Sun-like stars to roughly once per century.\\
-A few proposed generation mechanisms for superflares could be star-planet interaction (SPI) \citep{au_mic_flaring_spi,SPI_1,SPI_2}, or just being scaled up version of normal flares which we see from our Sun coming from large spots \citep{superflares_1,superflares_2}. In the case of the latter, we would expect to see a correlation between the appearance of superflares and the phase.\\
+A few proposed generation mechanisms for superflares could be star-planet interaction (SPI) \citep{au_mic_flaring_spi,SPI_1,SPI_2}, or just being scaled up version of normal flares which we see from our Sun coming from large spots \citep{superflares_1,superflares_2}. In the latter case, we would expect to see a correlation between the appearance of superflares and the spot modulation/phase (spots or spot groups rotating in and out of the visible disk of a star, periodically slightly dimming it).
+%Due to the possible longevity of spots, up to several months on the sun \citep{sunspots_overview}, it is possible to fold lightcurves \\
 
 \section{State of the art \label{sec:intro:goals}}