The PSI Planet-building Code: Multi-zone, Multi-use S. J. Weidenschilling PSI Retreat August 20,...
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The PSI Planet-building Code: Multi-zone, Multi-use
S. J. Weidenschilling
PSI RetreatAugust 20, 2007
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Hybrid Collisional Code
• Neither particle-in-a-box nor N-body
• Designed to treat radially extended swarm of bodies orbiting a star
• Large dynamic size range, from dust
grains to giant planets
• Both serial and parallel versions
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• Collisions and stirring occur when orbits overlap, even for different zones (not a series of separate particle-in-box simulations)
• Mutual gravitational stirring and dynamical friction (energy exchange) for bodies in crossing orbits
• Long-range perturbations by large bodies, even if orbits don’t overlap
• Explicit transport of mass between zones due to collisions, gas drag, tidal interactions with nebula, “shepherding” by massive bodies, etc.
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Discrete Bodies
• Bodies larger than threshold mass (~1024 g) are treated as discrete
• Allows late-stage simulations after large bodies have formed
• Individual values of M, a, e, i evolve with time• Interact with continuum by viscous stirring,
dynamical friction
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• Gravitational scattering of discrete bodies treated as stochastic events, allows impulsive changes in orbital elements
• Angular orbital elements assumed evenly distributed, scattering treated as 2-body interactions
• New version of serial code includes a symplectic N-body integrator
• Discrete bodies can be designated with specified masses and orbits (i.e., planets)
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Example Calculation: Accretion in Inner Solar System
• Planetesimal swarm 0.5 - 4 AU
• Swarm mass ~ 7 Earth masses
• Initial planetesimal diameter 1 km
• Fragments retained to d = 1/8 km
• Model time to 5 MY
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Collisional evolution of the asteroid belt: Dust production
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Collisional evolution of planetesimal swarm during migration of outer planets
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Under Development• Secular perturbations on planetesimals and
embryos due to giant planets or stellar companions
• Modeling circumstellar debris disks, including dust production over stellar lifetimes ~ > 10 My
• Extension to small particle sizes, with radiation pressure and Poynting-Robertson drag
• Parallel version with symplectic N-body integrator