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Lukas Winkler 2019-08-26 14:41:22 +02:00
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@ -5,12 +5,12 @@ One important question for planet formation is, how water got to the earth. The
\todo{citation needed}
\section{The perfect merging assumption}
%\section{The perfect merging assumption}
To better understand how this process works, large n-body simulations over the lifetime of the solar systems have been conducted\footnote{for example \cite{dvorakSimulation}}. Most of these neglect the physical details of collisions when two bodies collide for simplicity and instead assume that a perfect merging occurs. So the entire mass of the two progenitor bodies and especially all of their water (ice) is retained in the newly created body. Obviously this is a simplification as in real collisions perfect merging is very rare and most of the time either partial accretion or a hit-and-run encounter occurs.\footcite{CollisionTypes} Therefore, the amount of water retained after collisions is consistently overestimated in these simulations. Depending on the parameters like impact angle and velocity, a large fraction of mass and water can be lost during collisions.\footcite{MaindlSummary}
\section{Some other heading}
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%\section{Some other heading}
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To understand how exactly the water transport works, one has to find an estimation of the mass and water fractions that are retained during two-body simulations depending on the parameters of the impact.
First, I will be shortly describing the simulation setup, the important parameters and the post-processing of the results (Chapter \ref{chapter:simulations}). Next I will summarize the results of the simulations and their properties (Chapter \ref{chapter:results}). In the main section I will then be describing three different approaches to interpolate and generalize these results for arbitrary collisions (Chapter \ref{chapter:interpolations}).