Circumstellar dust analogues can be studied experimentally to determine their col- lisional behavior and their optical properties. These results affect simulations of circumstellar disks in various, substantial ways: Collision results determine how dust aggregates grow and how their aerodynamic properties change with time. This determines how solids move throughout the disk, how they accumulate, and how planetesimals might be formed. The optical properties determine the observational signature of these effects and allow us to constrain the spatial distribution of dust in disks, the sizes of the aggregates, as well as the temperature and optical depth of the dust emission. In this contribution, it is discussed how theoretical models and their predictions depend on laboratory results and what we learned about disks from high spatial resolution radio interferometry.
Keyphrases
- health risk assessment
- health risk
- human health
- polycyclic aromatic hydrocarbons
- heavy metals
- molecular dynamics
- risk assessment
- high speed
- high resolution
- climate change
- molecular docking
- monte carlo
- mass spectrometry
- optical coherence tomography
- solid state
- molecular dynamics simulations
- structure activity relationship