Numerical simulations of magnetic structures

I. N. Kitiashvili, A. G. Kosovichev, A. A. Wray, N. N. Mansour

Research output: Chapter in Book/Report/Conference proceedingConference contribution

Abstract

We use 3D radiative MHD simulations of the upper turbulent convection layer for investigation of physical mechanisms of formation of magnetic structures on the Sun. The simulations include all essential physical processes, and are based of the LES (Large-Eddy Simulations) approach for describing the sub-grid scale turbulence. The simulation domain covers the top layer of the convection zone and the lower atmosphere. The results reveal a process of spontaneous formation of stable magnetic structures from an initially weak vertical magnetic field, uniformly distributed in the simulation domain. The process starts concentration of magnetic patches at the boundaries of granular cells, which are subsequently merged together into a stable large-scale structure by converging downdrafts below the surface. The resulting structure represents a compact concentration of strong magnetic field, reaching 6 kG in the interior. It has a cluster-like internal structurization, and is maintained by strong downdrafts extending into the deep layers.

Original languageEnglish (US)
Title of host publicationThe Physics of Sun and Star Spots
EditorsDebi Prasad Choudhary, Klaus Strassmeier
Pages315-319
Number of pages5
EditionS273
DOIs
StatePublished - Aug 2010
Externally publishedYes

Publication series

NameProceedings of the International Astronomical Union
NumberS273
Volume6
ISSN (Print)1743-9213
ISSN (Electronic)1743-9221

All Science Journal Classification (ASJC) codes

  • Medicine (miscellaneous)
  • Astronomy and Astrophysics
  • Nutrition and Dietetics
  • Public Health, Environmental and Occupational Health
  • Space and Planetary Science

Keywords

  • Sun: magnetic fields
  • Sunspots; methods: numerical

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