Numerical Simulations of Solar Magneto-Convection

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Spontaneous pore formationStein 2012 Kitiashvili et al. 2010• No direct linkage to flux emergence• Form spontaneously if enough flux present in photosphere• No pore formation observed so far in SSD simulationsNSO Workshop 27 May 7-10, 2013
Recent progress in MHD modeling <strong>of</strong>sunspotsSchüssler & Vögler (2006) Heinemann et al. (2007)Scharmer et al. (2008)Kitiashvili et al. (2009)Rempel et al. (2009)NSO 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 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

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