On the Filamentary Nature of Solar Magnetic Fields

摘要: A method is presented for obtaining information about the unresolved filamentary structure of solar magnetic fields. comparison made pairs Mount Wilson magnetograph recordings in two spectral lines Fei 5250 and 5233 obtained on 26 different days. Due to line weakenings saturation filaments, apparent field strengths measured are too low, while expected give essentially correct results. From a between fluxes their center limb variations, we draw following tentative conclusions: (a) More than 90 % total flux seen with 17 by arc sec aperture channeled through narrow filaments very high plages at boundaries supergranular cells. (b) An upper limit interfilamentary strength integrated over same seems be 3 G. (c) The filament confined small region photosphere but spread out rapidly higher up atmosphere. (d) All earlier data should multiplied factor that 1.8 disk decreased toward order value longitudinal averaged scanning aperture.