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The Zeeman pattern of MnI lines is sensitive to hyperfine structure (HFS)and, they respond to hG magnetic field strengths differently from the linesused in solar magnetometry. This peculiarity has been employed to measuremagnetic field strengths in quiet Sun regions. However, the methods applied sofar assume the magnetic field to be constant in the resolution element. Theassumption is clearly insufficient to describe the complex quiet Sun magneticfields, biasing the results of the measurements. We present the first synthesesof MnI lines in realistic quiet Sun model atmospheres. The syntheses show howthe MnI lines weaken with increasing field strength. In particular, kG magneticconcentrations produce NnI 5538 circular polarization signals (Stokes V) whichcan be up to two orders of magnitude smaller than the weak magnetic fieldapproximation prediction. Consequently, (1) the polarization emerging from anatmosphere having weak and strong fields is biased towards the weak fields, and(2) HFS features characteristic of weak fields show up even when the magneticflux and energy are dominated by kG fields. For the HFS feature of MnI 5538 todisappear the filling factor of kG fields has to be larger than the fillingfactor of sub-kG fields. Stokes V depends on magnetic field inclinationaccording to the simple consine law. Atmospheres with unresolved velocitiesproduce asymmetric line profiles, which cannot be reproduced by simpleone-component model atmospheres. The uncertainty of the HFS constants do notlimit the use of MnI lines for magnetometry.

Quiet Sun Magnetic Field Measurements Based on Lines with Hyperfine Structure