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Solar Convection Simulations for Understanding Sun's Dynamics

Explore detailed simulations of solar convection, from magneto-convection to wave reflection, to study magnetic fields, velocity, and temperature fluctuations. Future simulations target active region fields and magnetic flux tubes for enhanced insights.

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Solar Convection Simulations for Understanding Sun's Dynamics

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  1. Solar Convection Simulations • Bob Stein • Åke Nordlund • Dali Georgobiani • Werner Schaffenberger • David Benson

  2. Current Simulations • Hydrodynamic-Convection96 Mm wide x 20 Mm deepResolution: 100 km horizontal, 12-75 km vertical20.9 hours • Magneto-Convection, 250G mean Bvertical6 Mm wide x -.5 to 2.5 Mm deepResolution: 6 km horizontal, 4.6 - 14 km vertical3.5 minutes

  3. Streamlines. 15 hours, 48 Mm wide x 20 Mm deep. Vertical scale is depth.

  4. Tracer particle motion. 15 hours, 48 Mm wide x 20 Mm deep. Vertical scale is grid (not depth).

  5. Wave Reflection - Characteristic BC Bottom Top

  6. Velocity at surface -- note swirls

  7. Magnetic field at surface (kG). <Bvert>=250 G

  8. Emergent continuum intensity

  9. Velocity slice (km/s)

  10. Vertical velocity (image) and Magnetic Field (vectors) in slice (km/s)

  11. Temperature fluctuation and Velocity in slice

  12. Vxy T Bxy T

  13. Future Simulations • Construct starting solution for 20 Mm deep run with characteristic BC (now) • Feed in horizontal magnetic field at bottom of 20 Mm deep x 48 Mm wide box to study network formation and maintenance (March 08) • Impose active region field on 96 Mm wide convection snapshot (May 08) • Feed in twisted magnetic flux tube at bottom of 20 Mm deep x 48 Mm wide simulation (May 08) Support: NNX07AO71G, NNX07AH79G, NNX07AI08G, AST0605738

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