% !TEX root = ../thesis-example.tex
%Example chapter on Asteroseismology
\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.

\section{Current knowledge \label{sec:intro:cur_knowledge}}

% motivation for the thesis

\section{Spectral Types \label{sec:intro:spectral_types}}

% Different Spectral Types

\section{Flares and Starspots \label{sec:intro:flares_and_spots}}

% Stellar Activity, 

\section{Space missions \label{sec:intro:space_missions}}

% TESS, Kepler/K2

\citet{Thompson2012}.

\begin{figure}[t!]
  \includegraphics[width=\linewidth]{gfx/rghbHRD.pdf}
  \caption{Position of the 18 red giant heartbeat stars from Tables 1 and 2 in
the HR diagram, where the colour shows the mass of the red giant, derived from seismology. The size of the dots represents the orbital period,
ranging between 20 and 438 d. The contour surfaces reflect the density
distribution of 1000 pulsating red giants. The darkest areas mark the
position of the densely populated red clump. Numbers in red indicate
the star count per bin, for which the contour surfaces have been drawn.
Lines of equal radii in the HR diagram have been drawn for selected
stellar radii between 5 and 30 R. \citep[Figure taken from][]{Beck2014}}
  \label{fig:singelPanelPlot}
\end{figure}

\textit{Kepler} \ref{sec:conclusion}

\begin{eqnarray}
c^2 &=& a^2 + b^2, \label{eq:pyth1}\\
c &=& \sqrt{a^2 + b^2} \label{eq:pyth2},
\end{eqnarray}
