Abstract
Under good seeing conditions (<2′), the high resolution magnetic field observation at Huairou Solar Observing Station'is capable of detecting the intranetwork field. An analysis of some magnetograms of 1988 September 5 shows: 1. That the observed weak intranetwork magnetic fields (WINF) with maximum flux B between 5 and 10 G are real structures. 2. That About 70% of the WINF became undetectable at ± 5 G level after 3.4 min and about 30% can be seen again. 3. That the number of WINF seen decreased exponentially with time, from which we estimated an upper limit of about 3 min for the mean life of a WINF. 4. That a WINF is a collection of unresolved flux elements, with a flux between 2.0(+16) and 1.0(+18) mx. Our results are similar to those in the magnetograms of 1984 September 9 obtained by the Big Bear Solar Observatory.
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