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 calculated from a Big Bear magnetogram obtained with moderately high spatial resolution of 1.5 arc sec and a high sensitivity reaching 2 Mx cm(-2). The effect of seeing on the power spectrum has been corrected using Fried's (1966) Modulation Transfer Function with the seeing parameter determined in our previous analysis of the magnetogram. As a result, it is found that the two-dimensional power spectra of network and non-network 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 Mm(-1) for network fields and k(0) approximate to 0.69 Mm(-1) for non-network fields, the latter of which corresponds to the size of mesogranulation; k(1) approximate to 3.0 Mm(-1) for both, which is about the size of a large granule. The network field spectrum below k(0) appears nearly flat, whereas that of non-network fields instead decreases towards lower wave numbers as Gamma(k) similar to k(1.3). The turnover behavior of magnetic field spectra around k(1) coincides with that found for the velocity power spectrum, which may justify the kinetic approach taken in previous theoretical studies of the solar magnetic power spectra.