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Journal of Physical Studies 14(2), Article 2903 [8 pages] (2010)
DOI: https://doi.org/10.30970/jps.14.2903 THE 2D MHD SIMULATION OF SOLAR MAGNETOGRANULATION: HORIZONTAL MAGNETIC FIELDSV. Sheminova
Astronomical Observatory, National Academy of
Sciences of Ukraine
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The solar horizontal magnetic fields on scales less than the spatial resolution of solar telescopes are investigated. A synthetic infrared spectropolarimetric diagnostics based on the 2D MHD simulation of magnetoconvection in а network region is used for this purpose. We find that the spatial average unsigned magnetic horizontal field strength at $ τ_5=1$ is 244 G and the most probable strength is equal to 50 G. The magnetic horizontal field surpasses by the factor 1.3, on average, the vertical field at the range of heights 0-400 km in the photosphere. It is caused by the stronger flux density of horizontal field and the larger area fraction occupied by them. Strong horizontal magnetic fluxes are visible on the surface in the form of small spots with the strength more than 500 G. The results of the Stokes diagnostics with respect to horizontal magnetic fields are qualitatively in agreement with that observed a board the ‟Hinode” satelite.
PACS number(s): 96.60.-j, 96.25.Ln, 96.60.Mz