ON THE DISTRIBUTION OF THE SOLAR MAGNETIC-FIELDS

This paper reports a study of the distribution of the solar magnetic f ield using the two magnetically sensitive infrared Fe I lines at 15648 Angstrom and 15652 Angstrom. We scanned the spectrograph slit across the solar surface (both active and quiet regions) to obtain three-dime nsional data cubes (two spatial dimensions and one spectral dimension) . Using the full Stokes V profiles, we can measure the true magnetic h eld strength the size, and the magnetic flux of magnetic elements simu ltaneously. The major findings of this observation can be summarized a s follows: 1. We made the first direct Zeeman splitting measurement of the intranetwork elements. The average field strength of the intranet work elements with a magnetic flux above 1.5 x 10(16) Mx per pixel is approximately 500 G. 2. To the first-order approximation, the surface magnetic field distribution can be described by a two-component model. The first component is the strong-field component. It has an average field strength of approximately 1400 G and is found in the sunspots, p lages, and network elements. The second component has intrinsically we aker field strength, typically around 500 G. It is found mostly in the intranetwork magnetic elements. 3. The average size of the weak-held elements is approximately 70 km in diameter. We suggest that the stron g-field component represents the large-scale, deeply rooted solar cycl e held, and the weak-field component originates in the solar convectio n zone, and may be generated from the turbulent velocity field by mixi ng and dispersion of floating strong flux tubes (U-loops) (Spruit, Tit le, and Van Ballegooijen 1987), and as a small-scale dynamo (Petrovay and Szakaly 1993; Durney, De Young, and Roxburgh 1993). We propose tha t the strong- and weak-held components are supported by the thermal an d turbulent pressure of the solar photosphere, respectively.