initial changes from overleaf

Physics_Thesis_Template/content/chapter-conclusion.tex

@@ -1,3 +1,3 @@
 \chapter{Conclusion and Outlook}
 \label{sec:conclusion}
-\lipsum[1-3]
+

Physics_Thesis_Template/content/chapter-data.tex

@@ -1,11 +1,26 @@
 % !TEX root = ../thesis-example.tex
 %
-\chapter{Methodology}
+\chapter{Data}
 \label{sec:data}
-\lipsum[1]
 
-\section{This is a section}
-\lipsum[2-4]
+This chapter will explain how the used data was gathered, as well as the criteria for which data was used for the final results. Lastly, I will describe the algorithms used.
+
+\section{Source}
+
+The data used in this thesis was gathered with the help of the astroquery (\cite{astroquery}) python package. For this purpose, as well as displaying the downloaded data, a GUI application was created with the python package PyQt5 (\cite{pyqt5}). The GUI window for downloads can be seen in \ref{fig:download_new_star_data_gui}. 
+
+\begin{figure}[pt!]
+  \includegraphics[width=\linewidth]{Physics_Thesis_Template/gui/download_star_data_gui.png}
+  \caption{GUI window for downloading new fit files with astroquery. }
+  \label{fig:download_new_star_data_gui}
+\end{figure}
+
+\section{Data selection}
+
+
+
+\section{Data reduction}
+
 
 \begin{table}[tp!]
 \caption{Training sample of false-positive planet candidates for the clustering algorithm.}
@@ -44,13 +59,13 @@ Reference \\
 \tablefoot{The star's identifier is given. For the most prominent stars, the name of the star is amended in brackets.  The next columns report on the effective temperature and the luminosity of the star in units of the solar luminosity L$_\odot$. The typical uncertainty of the reported temperature and luminosity are 150K and $\sim$10\%, respectively. The top and bottom panel report classification of the clustering. The cluster name refers to the position in the red-giant phase. The literature references are provided in the last column. (Table taken from Elisabeth Höldrich bachelor thesis, 2020)}
 \end{table}
 
-\lipsum[4]
+
 
 \subsection{This is a subsection}
-\lipsum[4]
+
 
 \section{Example of a code snippet \label{sec:MESA:Inlists}}
-\lipsum[1]
+
 
 
 \begin{table}[tp]
@@ -72,9 +87,6 @@ The keywords for defining the formalistic description for circularization and sy
 \end{table}
 
 
-\lipsum[2-3]
-
-
 \begin{figure}[pt!]
   \includegraphics[width=\linewidth]{gfx/spectralSegmentDisentanlging.pdf}
   \caption{Disentangled spectra of KIC 9163796. The spectra of the primary in blue and secondary in red are shown in the left and right spectrum,
@@ -84,8 +96,6 @@ line is shown depicted in the region of the Mg triplet. \citep[Graphic taken fro
   \label{fig:multiPanelPlot}
 \end{figure}
 
-\lipsum[3]
-
 
 \begin{landscape}
 \begin{table}[tp!]

Physics_Thesis_Template/content/chapter-discussion.tex

@@ -1,5 +1,3 @@
 \chapter{Discussion}
 \label{sec:discussion}
 
-\lipsum[1-7]
-

Physics_Thesis_Template/content/chapter-introduction.tex

@@ -3,7 +3,23 @@
 \chapter{Introduction \label{sec:intro}}
 %\cleanchapterquote{Shoot for the moon. Even if you miss, you'll land among the stars.}{Les Brown} %optional, if you want to place something here.
 
-Binary stars play a major role in astrophysics since their analysis by different means enables astronomers to deduce various stellar properties. In this thesis the binary system KIC 10614012 is analysed by combining asteroseismic techniques with radial velocity measurements and light curve analysis. This star system, also referred to as TYC 3561-1138-1, is part of the Kepler Input Catalog (KIC), a catalogue for potential target stars of the \textit{Kepler} mission. KIC 10614012 is an eclipsing binary (EB), i.e. an eclipse is visible in its light curve \citep[as written in][]{Kirk2016}. Furthermore, \cite{Beck2014} has shown that this star exhibits tidally induced flux modulations during periastron passage, on its eccentric ($e = 0.71$) orbit. Such binary stars, theorized by \citet{Kumar:1995}, are colloquially referred to as \textit{Heartbeat stars}, a term coined by \citet{Thompson2012}.
+\section{Current knowledge}
+
+% motivation for the thesis
+
+\section{Spectral Types}
+
+% Different Spectral Types
+
+\section{Flares and Starspots}
+
+% Stellar Activity, 
+
+\section{Spacecrafts}
+
+% TESS, Kepler/K2
+
+\citet{Thompson2012}.
 
 \begin{figure}[t!]
   \includegraphics[width=\linewidth]{gfx/rghbHRD.pdf}
@@ -18,15 +34,9 @@ stellar radii between 5 and 30 R. \citep[Figure taken from][]{Beck2014}}
   \label{fig:singelPanelPlot}
 \end{figure}
 
-This case study is divided into 7 sections. The first section (Sec.\,\ref{sec:intro}) gives a brief introduction into some of the underlying astrophysics of this analysis. Sec.\,\ref{sec:data} presents the three datasets used for this case study (light curves, asteroseismic power spectra and radial velocity measurements) and the instruments which obtained them (\textit{Kepler} and HERMES). The analysis of KIC 10614012 by means of asteroseismology is described in Sec.\,\ref{sec:data}, while the next chapter (Sec.\,\ref{sec:results}) deals with the system's analysis regarding its binary features. The fifth section (Sec.\,\ref{sec:results}) combines results from the previous two sections and estimates stellar properties of both, the primary and the secondary. A discussion of those results and a comparison to other studies are given in Sec.\,\ref{sec:discussion}. Eventually, in Sec.\,\ref{sec:conclusion} some conclusions are drawn, suggestions for further analysis of KIC 10614012 are given and a brief outlook on future prospects in asteroseismology is provided.
+\textit{Kepler} \ref{sec:conclusion}
 
-
-Calculating the hypotenuse follows the sentence of Pythagoras, 
 \begin{eqnarray}
 c^2 &=& a^2 + b^2, \label{eq:pyth1}\\
 c &=& \sqrt{a^2 + b^2} \label{eq:pyth2},
 \end{eqnarray}
-whereby $a$ and $b$ are the cathetus and $c$ the hypotenuse of a right-angled triangle. Please note that $a$ and $b$ are typically in the range of 10$^{-9}$\,$\lesssim$\,R/R$_\odot$\,$\lesssim$\,10$^6$.
-
-
-\lipsum[1]