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Adaptive Mesh Particle Simulator (AMPS)

Valeriy Tenishev, Dmitriy Borovikov , Nicolas Fougere , Yuni Lee, Michael R. Combi , Tamas Gombosi , Martin Rubin. Adaptive Mesh Particle Simulator (AMPS). Flare/CME Observations. SWMF Control & Infrastructure. Upstream Monitors. Eruption Generator. Radiation Belts. Energetic

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Adaptive Mesh Particle Simulator (AMPS)

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  1. Valeriy Tenishev, DmitriyBorovikov, Nicolas Fougere, Yuni Lee, Michael R. Combi, TamasGombosi, Martin Rubin Adaptive Mesh Particle Simulator (AMPS)

  2. Flare/CME Observations SWMF Control & Infrastructure Upstream Monitors Eruption Generator Radiation Belts Energetic Particles Polar Wind Magneto-grams, rotation tomography F10.7 Flux Gravity Waves Inner Heliosphere Thermosphere & Ionosphere Solar Corona 3D Outer Heliosphere Inner Magnetosphere Ionospheric Electrodynamics Particle Tracker Particle in Cell Radars Magnetometers In-situ New component of SWMF AMPS BATSRUS BATSRUS BATSRUS Couplers Global Magnetosphere IPIC3D BATSRUS

  3. AMPS • DSMC scheme • Realistic modeling of collisions in rarefied gas • Photochemical reactions for production of the minor species • Two phase simulation: gas and dust in a single model run • Adaptive mesh with cut-cells • Irregular nucleus shape for modeling the coma • Realistic shape model of Rosetta spacecraft for modeling of its gas environment • Variable mesh resolution to capture important features of the dusty gas flow • Integration with SPICE and SWMF

  4. Method and Applications • Non-equilibrium dusty gas flow • Comets, planetary satellites and exospheres • Common characteristic: the collision coupling cannot maintain the state of the equilibrium • Kinetic description • Boltzmann equation • The evolution of the system is modeled by tracing the model particles • Translational motion is separated from the particles collisions and chemistry

  5. Method • Translational particle motion • Particle collisions and chemistry • HS, VHS, VSS molecular models • TC, NTC, MF collision models • LB, QLB models of the internal degrees of freedom • Photo-ionization and photo-dissociation

  6. Method • Ion/neutral gas and dust • Modeled simultaneously • Optimizations • Local time step and particle weight • Individual particle weight correction • Domain decomposition • Load balancing • Static: volume, cell number • Dynamic: particle number, execution time

  7. Mesh • AMR with cut-cells

  8. Execution • Stand-along and a component of SWMF • Settings User-defined parameter file Generic AMPS’ core User-defined model routines

  9. Coupling with SWMF • New coupling scheme between AMPS and BATSRUS • One-way coupling in production runs

  10. Example • Na in Moon’s exosphere SPICE routines are integrated into AMPS. SPICE is used for calculating Moon’s orbital parameters, location of the spacecraft and pointing direction of the instrument. Sodium exospheric brightness. Comparison with observations obtained by UV instrument onboard Kaguya. Calculation of the column integrals are incorporated into AMPS.

  11. Example • New development: O2 and O2+ in Europa’s exosphere O2 number density. Produced via sputtering by the magnetospheric ions. The ions flux is derived form BATSRUS restart files O2+ number density. Produced ionization of O2. Newly created ions are traced in the fields exported from BATSRUS restart files

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