On The Discrepancy Of Coronal Magnetic Fields In Solar Optics And Radio

It is analysed the discrepancy about the coronal magnetic field between solar optic and solar radio using magnetic fibril concept with filling factor and fractal structure model. The magnetic field of ¸ 100 G considered in solar optics is mean value in a large scale, and that of ¸ 1000 G in solar should be the value of fine structures inside "macro" loop. I. INTRODUTION The magnetic field in the solar corona is poorly known because there are few kinds of observations that can measure it unambiguously (Gary et al.1993). It is contentious about the coronal magnetic fields in solar optics and radio. In solar optics, the magnetic field is usually considered as ¸ 100 G, many measurements indicate that few or no prominences have field strengths above 150 G, and typical strengths are 26 G (Harvey 1969); in solar radio, it is always takens as ¸ 1000 G to fit the observed emission flux, Peterson and Winckler (1959) took the field strength of 1000 G in calculating the number of fast electrons ..