1. Dust Flow in Disks in the presence of Embedded Planets
Sijme-Jan Paardekooper
Sterrewacht Leiden

2. Outline
Introduction
Disk models
Results
Conclusions and Future Work

3. Introduction Dust Dynamics Planet-Disk interaction Observing gaps
Angular momentum transport
Wolf et al. (2002): dust/gas = 0.01
Dust Dynamics

4. Disk Models Two-fluid (gas + dust) Locally isothermal H / r = 0.05
Constant surface density
Md  0.01 M๏
Dust / gas = 0.01
Dust size: 0.1 – 5.0 mm (spherical)

5. Disk Models
Drag Force
Dust Drift
Shocks
Epstein,

6. Results
Planet: 0.1 MJ
(no gap!)
Dust:1.0 mm

7. Results
Dependence on particle size
Grains > 0.15 mm create a gap

8. Results Dependence on planetary mass
Minimum mass for gap formation: 0.05 MJ

9. Conclusions
Medium sized planets can change the distribution of large particles dramatically
Gap formation occurs for planets more massive than 0.05 MJ
Particles larger than 150 μm participate

10. Future Work
Observational consequences
Dust-dust interaction