Formation and Early Evolution of Planetary Systems
Research output: Thesis › Doctoral Thesis (compilation)
All of my work relies heavily on computer modelling. I used hydrodynamic simulations of a shearing box inside a protoplanetary disk to determine the dust-to-gas ratio needed to trigger the streaming instability as a function of particle size. Similarly, the protoplanetary disk model is a one-dimensional hydrodynamic model that includes sink terms for photoevaporative outflows. The dynamical evolution of planetary systems occurs after planet formation is complete and the disk has fully dissipated. Dynamical simulations were performed with an N-body code designed for long-term modelling of planetary orbits.
My work has shown that the streaming instability is active for smaller particles than previously thought possible. I also found that in a protoplanetary disk, planetesimals begin to form early in the outer disk, where photoevaporation can more easily remove the gas component. As the disk evolves, planetesimal formation moves inward. From my dynamical simulations I am able to use present-day observations to estimate the probability that a habitable planet would have survived in a given planetary system, and I can estimate the masses of the planets that suffered ejections or collisions in that system.
|Research areas and keywords||
Subject classification (UKÄ) – MANDATORY
|Award date||2016 Nov 24|
|Place of Publication||Lund|
|State||Published - 2016 Oct|
Related research output
Research output: Contribution to journal › Article
2012/06/04 → 2016/11/24
European Commission - FP7
2012/01/01 → 2016/12/31
Project: Research › Individual research project