last changes

Physics_Thesis_Template/content/abstract.tex

@@ -9,19 +9,19 @@
 
 
 %\noindent
-\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 one would expect to find a correlation with the appearance of spots on the stars surface.
+\physbf{Context.~} In recent years detection of flares and superflares on stars gained a lot of attention, but the origin of superflares is still under debate. One possibility is that superflares are scaled up versions of normal flares, for which one would expect to find a correlation with the appearance of spots on the stars surface.
 \\[0.75em]
 %\noindent
 \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 (M, K, G, and F) using Kepler/K2 and TESS lightcurves.
 \\[0.75em]
 \noindent
-\physbf{Methods.~} Over 300 stars were analysed 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.
+\physbf{Methods.~} Over 300 stars were analysed 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 and the dependence of flare counts across the normalized phase are analyzed.
 \\[0.75em]
 \noindent
-\physbf{Results.~} The analysed stars are investigated according to their spectral type. 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. 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 a distinct spot dependence.
+\physbf{Results.~} The analysed stars are investigated according to their spectral type. 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. The only cumulative results which shows a significant spot dependence are those for G type stars. The results for K type stars show one significant peak in the 10 bin histogram. There was no significant spot dependence found for M type stars, even though some individual stars show a distinct spot dependence.
 \\[0.75em]
 \noindent
-\physbf{Conclusions.~} Investigations of spot to flare dependence from literature could be partially reproduced. It is furthermore found that the used flare algorithm as well as the sample of stars used for analysis affect the results. The present investigation has revealed that only G-type main-sequence stars show that a more spotted hemisphere produces also a larger number of flares.
+\physbf{Conclusions.~} Investigations of spot to flare dependence from literature could be partially reproduced. It is furthermore found that the used flare algorithm as well as the sample of stars used for analysis affect the results. The present investigation has revealed that only G-type main-sequence stars show a larger number of flares on a more spotted hemisphere.
 
 
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@@ -38,16 +38,16 @@
 
 
 %\noindent
-\physbf{Kontext.~} In den letzten Jahren hat die Detektion von Flares und Superflares auf Sternen viel Aufmerksamkeit bekommen, jedoch ist der Ursprung von Superflares immer noch umstritten. Eine Möglichkeit ist, dass Superflares nur stärkere Versionen von normalen Flares sind. In diesem Fall würde man eine Korrelation mit dem Auftreten von Flecken auf der Sternoberfläche erwarten.
+\physbf{Kontext.~} In den letzten Jahren hat die Detektion von Flares und Superflares auf Sternen viel Aufmerksamkeit erhalten, jedoch ist der Ursprung von Superflares immer noch umstritten. Eine Möglichkeit ist, dass Superflares energiereichere normale Flares sind. In diesem Fall wäre eine Korrelation mit dem Auftreten von Flecken auf der Sternoberfläche zu erwarten.
 \\[0.75em]
 %\noindent
-\physbf{Ziele.~} Das Ziel dieser Studie ist es Flares und Superflares und das Auftreten von Flecken auf Sternoberflächen verschiedener Spektraltypen (M, K, G, und F) in relation zu bringen. Dafür wurden Lichtkurven von Kepler/K2 und TESS verwendet.
+\physbf{Ziele.~} Das Ziel dieser Studie ist es Flares und Superflares und das Auftreten von Flecken auf Sternoberflächen verschiedener Spektraltypen (M, K, G, und F) in Relation zu bringen. Dafür wurden Lichtkurven von Kepler/K2 und TESS verwendet.
 \\[0.75em]
 \noindent
-\physbf{Methoden.~} Es wurden über 300 Sterne mit einer neu entwickelten GUI-Anwendung und Flareerkennungsalgorythmus analysiert, welcher Flares mit normalisierten Spitzenwerten von 0.3\% über dem Umgebungsfluss erkennen kann. Die Lichtkurven werden danach mit einer automatisch erkannten Fleckenmodulationsperiode gefalten.
+\physbf{Methoden.~} Es wurden über 300 Sterne mit einer neu entwickelten GUI-Anwendung und einem Flareerkennungsalgorithmus analysiert, welcher Flares mit normalisierten Spitzenwerten von 0.3\% über dem Umgebungsfluss erkennen kann. Die Lichtkurven werden danach mit einer automatisch erkannten Fleckenmodulationsperiode gefaltet und die Abhängigkeit der Flareanzahl von der normalisierten Phase wurde analysiert.
 \\[0.75em]
 \noindent
 \physbf{Ergebnisse.~} Die analysierten Sterne wurden anhand ihres Spektraltyps untersucht. Wir präsentieren auch einzelne Ergebnisse für die Sterne BD-08 995, TYC 1360-957-1, TYC 4595-107-1, V* V471 Tau, V* HK Aqr, KOI-256 und 2MASS J19230963+3739397. Die einzige signifikante Fleckenabhängigkeit wurde bei den Gesamtergebnissen für G-Sterne gefunden. Die Ergebnisse für K-Sterne zeigen einen signifikanten Spitzenwert im Histogramm mit 10 Bins. Für M-Sterne wurde keine signifikante Abhängigkeit gefunden, obwohl ein paar Einzelsterne eine Abhängigkeit aufweisen.
 \\[0.75em]
 \noindent
-\physbf{Fazit.~} Untersuchungen aus der Literatur konnten teilweise nachgewiesen werden. Weiters wurde herausgefunden, dass sowohl der Flareerkennungsalgorythmus als auch die Auswahl an analysierten Sternen einen Einfluss auf das Ergebnis hat. Die derzeitige Untersuchung hat gezeigt, dass nur G-Sterne der Hauptreihe eine erhöhte Anzahl an Flares auf einer fleckenreicheren Hemisphäre zeigen.
+\physbf{Fazit.~} Ähnliche Untersuchungen aus der Literatur konnten teilweise reproduziert werden. Darüber hinaus wurde ermittelt, dass sowohl der Flareerkennungsalgorithmus als auch die Auswahl an analysierten Sternen einen Einfluss auf das Ergebnis haben. Die derzeitige Untersuchung hat gezeigt, dass nur Hauptreihensterne vom Spektraltyp G eine erhöhte Anzahl an Flares auf einer fleckenreicheren Hemisphäre zeigen.

Physics_Thesis_Template/content/chapter-discussion.tex

@@ -36,4 +36,4 @@ A similar finding was made on HK Aqr. Also the three strongest flares have been
 Looking at all results together, there is a trend that more flares occur when a more spotted stellar hemisphere is visible, than vice versa. This is mostly influenced by the results for K and G stars. The dip in the otherwise seemingly flat histogram for the results of M dwarfs dominates the overall results.
 There is at the moment no explanation for the significant dip in the histogram and we doubt that it has a physical meaning.
 
-All results will be published on github. The program will be available at \url{https://github.com/SGCMarkus/flaredetector} while the data will be available at \url{https://github.com/SGCMarkus/flaredetector\_results}. The different branches define which fitting function was used for the data, e.g. the results containing all plots which used a sine function to fit, are found in the "sine" branch on Github.
+All results will be published on github. The program will be available at \url{https://gitlab.com/SGCMarkus/flaredetector} while the data will be available at \url{https://gitlab.com/SGCMarkus/flaredetector\_results}. The different branches define which fitting function was used for the data, e.g. the results containing all plots which used a sine function to fit, are found in the "sine" branch on Github.

Physics_Thesis_Template/content/chapter-results.tex

@@ -2,7 +2,7 @@
 
 This chapter includes the main results of this study. The data for the plots in this section were generated using the "New FC" Button from the main GUI described in section \ref{sec:gui:data_processing}. As every star has a different rotational/spot modulation period, the value range for the phases of the folded lightcurves do not match. To compare different stars (or spot modulation periods for the same star) with each other, the phase was normalized from $0$ to $2 \pi$.
 
-The results contain plots for the different spectral types M, K, G, and F as well as combined results of every possible combination. Additionally for all these possible combinations, plots with data limits, e.g. only stars with a rotational period of less than 2 days or minimal/maximal normalized flare peak limits, were also generated. Moreover plots for stars according to their spectral sub type like M0 or G5 were created. Furthermore there is a selection of individual star results. For every plot group a CSV file is generated, which contains information about every star and flare used to generate the plot. The results also only contain the data of folded lightcurves which could be fitted with a sine function and less than 30 iterations of the fold optimization. The data which uses polynomial fits or both sine and polynomial fits as well as all plots and the accompanying CSV files are available at \url{https://github.com/SGCMarkus/flaredetector\_results}.
+The results contain plots for the different spectral types M, K, G, and F as well as combined results of every possible combination. Additionally for all these possible combinations, plots with data limits, e.g. only stars with a rotational period of less than 2 days or minimal/maximal normalized flare peak limits, were also generated. Moreover plots for stars according to their spectral sub type like M0 or G5 were created. Furthermore there is a selection of individual star results. For every plot group a CSV file is generated, which contains information about every star and flare used to generate the plot. The results also only contain the data of folded lightcurves which could be fitted with a sine function and less than 30 iterations of the fold optimization. The data which uses polynomial fits or both sine and polynomial fits as well as all plots and the accompanying CSV files are available at \url{https://gitlab.com/SGCMarkus/flaredetector\_results}.
 
 \section{M dwarfs \label{sec:results:m_dwarfs}}
 

Physics_Thesis_Template/content/titlepages.tex

@@ -1,19 +1,19 @@
 % !TEX root = ../thesis-example.tex
 %
 
-% ------------------------------------  --> cover title page
+% % ------------------------------------  --> cover title page
-\begin{titlepage}
+% \begin{titlepage}
-	\pdfbookmark[0]{Cover}{Cover}
+% 	\pdfbookmark[0]{Cover}{Cover}
-	\flushright
+% 	\flushright
-	\hfill
+% 	\hfill
-	\vfill
+% 	\vfill
-	{\color{ctgreenblue}\LARGE\thesisTitle \par}
+% 	{\color{ctgreenblue}\LARGE\thesisTitle \par}
-	{\color{ctcolorgray}\large\thesisSubtitle}
+% 	{\color{ctcolorgray}\large\thesisSubtitle}
-	\color{ctgreenblue}\rule[5pt]{\textwidth}{1.25pt} \par
+% 	\color{ctgreenblue}\rule[5pt]{\textwidth}{1.25pt} \par
-	{\color{ctgreenblue}\Large\thesisName}
+% 	{\color{ctgreenblue}\Large\thesisName}
-	\vfill
+% 	\vfill
-	\textit{\large\thesisDate}
+% 	\textit{\large\thesisDate}
-\end{titlepage}
+% \end{titlepage}
 % ------------------------------------  --> page 2 left empty on purpose
 
 %\input{content/titlepageKFU} % uncomment for KFU style
@@ -29,7 +29,7 @@
 	\physbf{\thesisName} \\
 	\physit{\thesisTitle~$-$~\thesisSubtitle} \\[0.5em]
 	Thesis in partial fulfillment of the \hbox{requirements for the degree of \thesisDegree}; \\
-	Thesis submitted on \red{June DD, 2025}, and defended on \red{July 10, 2025}. %e.g. 2020, November 15, 2020. Before submission, uncomment this line, fill out the date, remove the red color of the data and delete the following line, containing 'Unsubmitted Thesis Manuscript'.
+	Thesis submitted on June 11, 2025, and defended on July 10, 2025. %e.g. 2020, November 15, 2020. Before submission, uncomment this line, fill out the date, remove the red color of the data and delete the following line, containing 'Unsubmitted Thesis Manuscript'.
 	%\red{\bfseries Unsubmitted Thesis Manuscript: compiled on \thesisDate}  
 	\\[0.5em]
 	Institute of Physics, NAWI Graz, University of Graz.\\[1.5em]