Solar convection and magneto-convection simulations

Stein, R.F. and Bercik, D. and Nordlund, A. (2002) Solar convection and magneto-convection simulations. Il nuovo cimento C, 25 (5\6). pp. 513-522. ISSN 1826-9885

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Magneto-convection simulations with two scenarios have been performed: in one, horizontal magnetic field is advected into the computational domain by fluid entering at the bottom. In the other, an initially uniform vertical magnetic field is imposed on a snapshot of non-magnetic convection and allowed to evolve. In both cases, the field is swept into the intergranular lanes and the boundaries of the underlying mesogranules. The largest field concentrations at the surface reach pressure balance with the surrounding gas. They suppress both horizontal and vertical flows, which reduces the heat transport. They cool, become evacuated and their optical depth unity surface is depressed by several hundred kilometers. Micropores form, typically where a small granule disappears and surrounding flux tubes squeeze into its previous location.

Item Type: Article
Additional Information: Paper presented at the International Meeting on THEMIS and the New Frontiers of Solar Atmosphere Dynamics, Rome, Italy, March 19-21, 2001.
Uncontrolled Keywords: Convection, turbulence, and diffusion ; Photoshere, granulation ; Conference proceedings
Subjects: 500 Scienze naturali e Matematica > 530 Fisica > 538 Magnetismo
Depositing User: Marina Spanti
Date Deposited: 12 Mar 2020 14:18
Last Modified: 12 Mar 2020 14:18

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