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Image: ISAS/JAXA

Collisional Grooming:. Including Collisions in (Prohibitively Large) N-body Simulations. Christopher Stark University of Maryland NASA Goddard Space Flight Center. Image: ISAS/JAXA. Fomalhaut.  Eri. Kalas et al. 2005. HR 4796A. Greaves et al. 1998. Schneider et al. 2009.

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Image: ISAS/JAXA

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  1. Collisional Grooming: Including Collisions in (Prohibitively Large) N-body Simulations Christopher Stark University of Maryland NASA Goddard Space Flight Center Image: ISAS/JAXA

  2. Fomalhaut  Eri Kalas et al. 2005 HR 4796A Greaves et al. 1998 Schneider et al. 2009

  3. Kalas et al. 2008

  4. Fomalhaut  Eri Kalas et al. 2005 HR 4796A Greaves et al. 1998 Schneider et al. 2009

  5. Velocity Dispersion in a Structured Debris Disk

  6. Planetary gravitational forces Radiation pressure Stellar gravitational force PR + solar wind drag

  7. The Collisional Grooming Algorithm Ni(t=t) = Ni(t=0)e- i Ni(t=2t) = Ni(t=t)e- i Ni = Ni(t=0) Ni(t=3t) = Ni(t=2t)e- i

  8. Iterative Convergence of the Collisional Grooming Algorithm

  9. Correctness of Solution to the Mass Flux Equation

  10. Collision Rate in a Resonant Ring Structure

  11. Collision Rate in a Resonant Ring Structure

  12. No Collisions More Collisions

  13. Fragmentation Ni(t=t) = Ni(t=0)e- i Ni = Ni(t=0)

  14. Fragmentation

  15. Fomalhaut  Eri Kalas et al. 2005 HR 4796A Greaves et al. 1998 Schneider et al. 2009

  16. Distribution of KBOs

  17.  = 0.6 m

  18.  = 60 m

  19.  = 800 m

  20. Disk-Total Grain Size Distribution

  21. Summary • Collisional grooming allows us to include gravitational resonant dynamics and grain-grain collisions simultaneously & self-consistently • Algorithm runs post-integration & takes ~1 hour on a single processor • Grain-grain collisions play an important role in determining debris disk morphology, even for disks with optical depths ~10-7

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