FLUX DISTRIBUTION OF SOLAR INTRANETWORK MAGNETIC-FIELDS

Big Bear deep magnetograms of June 4, 1992 provide unprecedented obser vations for direct measurements of solar intranetwork (IN) magnetic fi elds. More than 2500 individual IN elements and 500 network elements a re identified and their magnetic flux measured in a quiet region of 30 0 x 235 are sec. The analysis reveals the following results: (1) IN el ement flux ranges from 10(16) Mr (detection limit) to 2 x 10(18) Mr, w ith a peak flux distribution of 6 x 10(16) Mr. (2) More than 20% of th e total flux in this quiet region is in the form of IN elements at any given time. (3) Most IN elements appear as a cluster of mixed polarit ies from an emergence center (or centers) somewhere within the network interior. (4) The ZN flux is smaller than the network flux by more th an an order of magnitude. It has a uniform spatial distribution with e qual amount of both polarities. It is speculated that IN fields are in trinsically different from network fields and may be generated from a different source as well.