Numerical Simulations of Solar Magneto-Convection

More documents

Recommendations

Info

Field strength <strong>of</strong> quiet sun?• Depends on bottom boundary condition– B=0, B vertical, B isotropic …?• Upper limit:– B rms should not increase faster with depth than B eq• Lower Limit:– Assume B=0 in all inflow regions• Field strength range: ~30-80 G– Best match with Hinode data ~60 G(Danilovic & Rempel in prep.)NSO Workshop 27 May 7-10, 2013
From granulation to supergranulation• Domain size: 25x25x7.5 Mm 3 , resolution 16x16x16 km 3– Mesogranular magnetic field structure• Longer lived field concentrations and “voids”– Small-scale bipolar flux emergenceNSO Workshop 27 May 7-10, 2013
Page 1: Numerical Simulations of SolarMagne
Page 5 and 6: Sun at 2 km resolution• Simulatio
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 22 and 23: Sunspot fine structure (at tau=1)NS
Page 24 and 25: MHD simulations and helioseismology

Numerical Simulations of Solar Magneto-Convection

You also want an ePaper? Increase the reach of your titles

Delete template?

Save as template?