Speaker
Description
Planet formation is an important topic, but how planets are forming in protoplanetary disks is still not fully understood. Silicate monomers (um-sized) are present in the disk and may attach to each-other to form fluffy, porous aggregates, which may then further progress into more solid pebbles, into planetesimals or protoplanets through a variety of proposed pathways. The material properties of these fluffy aggregates are still being researched, and may have a significant impact on the viability of various proposed pathways for planet formation. In order to investigate these material properties, both physical experiments and theoretical simulations are necessary. As part of a broader effort, this work aims to investigate the effectiveness of smoothed particle hydrodynamics (SPH) simulations in describing and predicting fluffy aggregate material properties, in particular with respect to porosity change through collisions.
The work to be presented at the conference includes comparisons of the simulation results under various proposed equations of state for dust aggregates, an evaluation of the applicability of SPH on these proposed physical models, and its viability in modelling experimental results to help determine which physical models are most consistent with observations.
| Talk category | NOVA Network 2 |
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