POWER SPECTRA OF SOLAR NETWORK AND NON-NETWORK FIELDS

We report new properties of solar magnetic fields in a quiet region as found from their magnetic power spectra. The power spectra of network and intranetwork fields (non-network fields) are separately calculate d from a Big Bear magnetogram obtained with moderately high spatial re solution of 1.5 arc sec and a high sensitivity reaching 2 Mx cm(-2). T he effect of seeing on the power spectrum has been corrected using Fri ed's (1966) Modulation Transfer Function with the seeing parameter det ermined in our previous analysis of the magnetogram. As a result, it i s found that the two-dimensional power spectra of network and non-netw ork fields appear in a form: Gamma(k(0) less than or similar to k less than or similar to k(1)) similar to k(-1) and Gamma(k greater than or similar to, k(1)) similar to k(-3.5). Here k(0) approximate to 0.47 M m(-1) for network fields and k(0) approximate to 0.69 Mm(-1) for non-n etwork fields, the latter of which corresponds to the size of mesogran ulation; k(1) approximate to 3.0 Mm(-1) for both, which is about the s ize of a large granule. The network field spectrum below k(0) appears nearly flat, whereas that of non-network fields instead decreases towa rds lower wave numbers as Gamma(k) similar to k(1.3). The turnover beh avior of magnetic field spectra around k(1) coincides with that found for the velocity power spectrum, which may justify the kinetic approac h taken in previous theoretical studies of the solar magnetic power sp ectra.