ROTATIONAL CHARACTERISTICS OF THE GREEN SOLAR CORONA : 1947-1991

Fe XIV 530.3 nm coronal emission line observations have been used for the estimation of the green solar corona rotation. A homogeneous data set, created from measurements of the world-wide coronagraphic network, has been examinated with a help of correlation analysis to reveal the averaged synodic rotation period as a function of latitude and time over the epoch from 1947 to 1991. The values of the synodic rotation period obtained for this epoch for the whole range of latitudes and a latitude band 1#130⁰ are 27.521#10.12 days and 26.951#10.21 days, resp. A differential rotation of green solar corona, with local period maxima around 1#160⁰ and minimum of the rotation period at the equator, was confirmed . No clear cyclic variation of the rotation has been found for examinated epoch but some monotonic trends for some time intervals are presented. A detail investigation of the original data and their correlation functions has shown that an existence of sufficinetly reliable tracers is not evident for the whole set of examinated data. This should be taken into account in future more precise estimations of the green corona rotation period. Sun - corona - green emission line - rotation