From pebble to planet The growth, rotation and structure of planetary bodies formed from pebbles

In this thesis, I focus on the formation process and the resulting rotation that follows for planetesimals also called planets-in-formation (about 100 to 500 kilometers in radius) and larger planets (about 500 to 2000 kilometers in radius). In Chapter 2, the focus is on the time scale required to form the larger planets with pebble accretion. In Chapter 3 I use the same model but no longer look at growth but the rotation that pebbles give when they land on the planet-in-formation. Chapter 4 is about the stage of formation for the planet-in-formation. We think these form because the pebbles in the protoplanetary disk accumulate and cluster by interacting with the gas. This process is called Streaming Instability. I then look when it is formed by the collapse what the size distribution of pebbles in the core is because they are not all the same size and therefore will form a certain structure in the core during collapse.
In Chapter 5, I again look at rotation resulting from the process, in this case resulting from the gravitational collapse. These simulations are done in the framework of the central mass around which all pebbles revolve during collapse. Finally, in Chapter 5 I determine the growth and evolution of a binary system that forms due to, for example, streaming instability and then sweeps up pebbles during pebble accretion.