1 / 34

Dust crystallinity and the evolution of dusty disks

Dust crystallinity and the evolution of dusty disks. C.P. Dullemond, D. Apai, A. Natta, L. Testi, C. Dominik, S. Walch. Two questions:. What is the origin of the observed M ~ M * 2 relation of protoplanetary disks?. What does crystallinity of dust tell us about the processes in disks?.

qamar
Download Presentation

Dust crystallinity and the evolution of dusty disks

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Dust crystallinity andthe evolution of dusty disks C.P. Dullemond, D. Apai, A. Natta, L. Testi, C. Dominik, S. Walch

  2. Two questions: What is the origin of the observed M ~ M*2 relation of protoplanetary disks? What does crystallinity of dust tell us about the processes in disks?

  3. One answer: The process of disk formation and viscous evolution!

  4. Model • Start with a molecular cloud core of mass Mcore, effective sound speed cs, and rotation rate . • Use cloud collapse model to compute infall rate, and the radius within which this matter falls onto disk (Rcentr). • Use viscous evolution model to follow the disk evolution.

  5. Initial conditions of collapse: • Let’s take a simple Shu-type collapse: • Collapse starts from slowly rotating singular isothermal sphere • Mass-radius relation: • Infall rate constant: • Centrifugal radius:

  6. Mass conservation: Angular momentum conservation: Disk formation and spreading Let’s make a numerical model of the disk evolution:

  7. Disk formation and spreading

  8. Disk formation and spreading

  9. Disk formation and spreading

  10. Disk formation and spreading

  11. Disk formation and spreading

  12. Class II Class O, I Evolution of disk parameters (after Hueso & Guillot 2005)

  13. Correlation M - M*

  14. Accretion rate versus star mass Natta et al. 2005

  15. Accretion rate versus star mass • So let’s do an experiment: • Make numerical models for series of cores with ascending mass • Define dimensionless  (important!) (i.e. fraction of breakup rotation of core) • We assume  of the core NOT to depend on Mcore.

  16. Accretion rate versus star mass

  17. Disk mass versus star mass

  18. Crystallinity of dust

  19. 10-micron feature of crystalline dust Bouwman et al. 2001

  20. Crystalline silicates produced here (thermal annealing)... ...but they are observed here Turbulent transport Radial mixing Accretion Morfill & Völk (1984), Gail (2001) Wehrstedt & Gail (2002)

  21. New idea:

  22. New idea:

  23. New idea:

  24. Disk formation and spreading

  25. Disk formation and spreading

  26. Disk formation and spreading

  27. Disk formation and spreading

  28. Disk formation and spreading

  29. Evolution of crystallinity

  30. Evolution of crystallinity

  31. Evolution of crystallinity

  32. Evolution of crystallinity

  33. Evolution of crystallinity

  34. Summary • Self-consistent disk formation and evolution models: • can explain the M ~ M2 relation. • provide a new view to dust crystallinity • New problem: Why are there no 100% crystalline disks observed?

More Related