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Magnetic-field structure of the photospheric network

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Abstract

A method is developed to determine the physical parameters of the spatially unresolved photospheric network. The apparent magnetic fluxes are recorded simultaneously in the two FeI lines 5250 and 5247 Å, which belong to the same multiplet and have practically the same oscillator strength and excitation potential of the lower level, but differ in the effective Lande factor. By analysing magnetograph recordings in this pair of lines together with simultaneous recordings in the two FeI lines 5250 and 5233 Å, it is possible to separate the effects on the line profiles due to Zeeman splitting and temperature enhancement in the network.

From an analysis of the observations the following properties of the photospheric network are obtained: Field strengths of about 2000 G are present in the network in quiet regions. The characteristic size of the magnetic-field structures in the network appears to be in the range 100–300 km. The 5250 Å line is weakened by roughly 50% in the network. If the line had been non-magnetic, the weakening would have been about 20%. The rest of the weakening is caused by the strong Zeeman splitting. The downward velocity at the supergranular cell boundaries is estimated to be of the order of 0.5 km s-1.

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Authors and Affiliations

  1. Lund Observatory, Svanegatan 9, S-222 24, Lund, Sweden

    J. O. Stenflo

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  1. J. O. Stenflo
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Stenflo, J.O. Magnetic-field structure of the photospheric network. Sol Phys 32, 41–63 (1973). https://doi.org/10.1007/BF00152728

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  • DOI: https://doi.org/10.1007/BF00152728

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