GOALS

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GOALS

• Simulators tell Observers what we can do, are
  doing and plan to do
• Observers tell Simulators what they should do
  that would be useful to Observers
• Keep brief presentations to strict time limits
• Bob Stein - surface convection
• Mark Miesch - interior convection
• Nagi Mansour - wave propagation
• Junwei Zhao - time distance seismology
• Brad Hindman - ring diagram seismology
• Charlie Lindsey - holographic seismology
• General discussion after presentations
• Summary - Sasha Kosovichev

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Supergranulation SimulationDensity
fluctuation48x48x20 Mm
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simulation
MDI
Zhao Georgobiani
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Time-Distance Diagrams
Zhao Georgobiani
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Horizontal Velocity spectrum, (kP(k))1/2






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Velocity Spectrum - MDI datasupersonic/subsonic
filtered
kP(k)1/2
convection
oscillations
time averaged velocity
Velocity
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Emerging Flux

• Size of domain
• 24 by 2.3 by 12 Mm
• Initial flux tube properties
• Longitudinal flux 1019 Mx
• B0 8500 G
• Internal plasma beta1
• Twisted, B?/Bl 0.5 at r 200 km
• Specific entropy s value at base of solar
  convection zone

Cheung, Schüssler Moreno-Insertis
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G-band Magnetic Field
Contours .5, 1, 1.5 kG (gray) 20 G (red/green)
Initial uniform vertical fieldb250 G
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Plans

• Supergranule scale magneto-convection (in
  progress) 48 Mm wide x 20 Mm deep, includes
  surface shear layer Quiet Sun - magnetic
  network, flux emergence, dispersal Active
  region - extend surface vector magnetogram down
• Meso-granule scale magneto-convection plage
  region - mean vertical magnetic field 6 Mm wide
  x 3 Mm deep Hign resolution - 6 km horizontal
  vertical at surface Similar models by
  Schusler/Vogler et al.