Polarized radiation diagnostics of magnetohydrodynamic models of the solar atmosphere |
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Authors: | O Steiner U Grossmann-Doerth M Schüssler M Knölker |
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Institution: | (1) Kiepenheuer-Institut für Sonnenphysik, Schöneckstrasse 6, D-79104 Freiburg, Germany;(2) High Altitude Observatory, NCAR, P.O. Box 30000, 80307 Boulder, CO, USA |
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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
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.The National Center for Atmospheric Research is sponsored by the National Science Foundation |
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Keywords: | Magnetohydrodynamics Polarization Solar Atmosphere |
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