Abstract
Simultaneous observations of chromospheric (Hβ) and photospheric (Fe i λ5324.19 A) magnetograms in quiet solar regions enable us to study the spatial configuration of the magnetic field in the solar atmosphere. With the typical spatial resolution of the Huairou magnetograph, the photospheric and chromospheric magnetic structures of the quiet Sun maintain a very similar pattern. Moreover, the vertical magnetic flux is almost the same from the photosphere to the chromosphere. As an intermediate step, we analyze the formation of the working lines used by the Huairou video magnetograph of the Beijing Astronomical Observatory. The Stokes V contribution function of Hβ and Fe i λ5324.19 A are calculated. It is found that our Hβ magnetograms provide the distribution of the chromospheric magnetic field at a height some 1000–1500 km above the photosphere.
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