image: isas/jaxa christopher stark university of maryland nasa goddard space flight center...
TRANSCRIPT
Image: ISAS/JAXA
Christopher StarkUniversity of Maryland
NASA Goddard Space Flight Center
Collisional Grooming:
Including Collisions in (Prohibitively Large)N-body Simulations
Fomalhaut
Kalas et al. 2005
Greaves et al. 1998
Eri
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Schneider et al. 2009
HR 4796A
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Kalas et al. 2008
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Fomalhaut
Kalas et al. 2005
Greaves et al. 1998
Eri
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Schneider et al. 2009
HR 4796A
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Velocity Dispersion in a Structured Debris Disk
PR + solarwind drag
Stellargravitational
force
Planetarygravitational
forces Radiation pressure
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Ni = Ni(t=0)
Ni(t=t) = Ni(t=0)e-
Ni(t=2t) = Ni(t=t)e-
Ni(t=3t) = Ni(t=2t)e-
i
i
i
The Collisional Grooming Algorithm
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Iterative Convergence of the Collisional Grooming Algorithm
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Correctness of Solution to the Mass Flux Equation
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Qu
ickTim
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and a
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.Collision Rate in a Resonant Ring Structure
Collision Rate in a Resonant Ring Structure
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No Collisions More Collisions
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Ni = Ni(t=0)
Ni(t=t) = Ni(t=0)e- i
Fragmentation
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Fragmentation
Fomalhaut
Kalas et al. 2005
Greaves et al. 1998
Eri
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Schneider et al. 2009
HR 4796A
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Distribution of KBOs
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= 0.6 m
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= 60 m
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= 800 m
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Disk-Total Grain Size Distribution
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Summary
• Grain-grain collisions play an important role in determining debris disk morphology, even for disks with optical depths ~10-7
• 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