Numerical Simulations of Solar Magneto-Convection

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Sunspot fine structure (at tau=1)NSO Workshop 27 May 7-10, 2013

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Sunspot fine structure (at tau=1)NSO Workshop 27 May 7-10, 2013

The magnetoconvection pictureSide viewCentral upflow−rho (v grad) vBx, BzByVx, VzVyzytau=1x−grad p + rho gjxBBVzLateral downflowyPenumbral filament in MHD simulationupdownTop viewxyCross SectionNSO Workshop 27 May 7-10, 2013

Page 1: Numerical Simulations of SolarMagne
Page 5 and 6: Sun at 2 km resolution• Simulatio
Page 8 and 9: Field strength of quiet sun?• Dep
Page 10 and 11: From granulation to supergranulatio
Page 12 and 13: Power spectrum from 2km to 100Mm•
Page 14 and 15: Spontaneous pore formationStein 201
Page 16 and 17: The imagecannot bedisplayed.Yourcom
Page 18 and 19: Subsurface field structure?Monolith
Page 20 and 21: Simple model: Flows around obstacle
Page 24 and 25: MHD simulations and helioseismology

Numerical Simulations of Solar Magneto-Convection

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