Abstract
Solar magnetic elements and their dynamical interaction with the convective surface layers of the Sun are numerically simulated. Radiation transfer in the photosphere is taken into account. A simulation run over 18.5 minutes real time shows that the granular flow is capable of moving and bending a magnetic flux sheet (the magnetic element). At times it becomes inclined by up to 30° with respect to the vertical around the level τ 5000 = 1 and it moves horizontally with a maximal velocity of 4 km/s. Shock waves form outside and within the magnetic flux sheet. The latter cause a distinctive signature in a time series of synthetic Stokes V-profiles. Such shock events occur with a mean frequency of about 2.5 minutes. A time resolution of at least 10 seconds in Stokes V recordings is needed to reveal an individual shock event by observation.
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The National Center for Atmospheric Research is sponsored by the National Science Foundation
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Steiner, O., Grossmann-Doerth, U., Schüssler, M. et al. Polarized radiation diagnostics of magnetohydrodynamic models of the solar atmosphere. Sol Phys 164, 223–242 (1996). https://doi.org/10.1007/BF00146636
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DOI: https://doi.org/10.1007/BF00146636