ROTATION OF THE SOLAR GREEN CORONA -
TRACER RESULTS AND THEIR RELIABILITY

Abstract

All available patrol measurements of intensities of the solar green coronal emission line have been used for a reliability test of the results of corona rotation. This was done with help of the tracer method comparing the results from relatively independent measurements on the east and west limbs. The differences of the synodic rotational periods less than 1 day can be seen for 521#1 of the investigated time-latitude domain over the epoch of 45 years and the latitude range of 2#2803#3, when a careful selection of available tracers is applied.

The emission corona changes rapidly its latitude behaviour over solar cycles from high rigidity during solar minima to a differential shape two years after and during cycle maxima, and then more slowly to the former behaviour. General latitude behaviour of the rotational period of the emission corona for higher (>603#3) heliographic latitudes is influenced by a selection effect and no satisfactory precise determination can be presented. For lower latitudes the averall rotation is discussed and its approximation is inferred.

It is concluded that the rotation information, inferred from time-latitude areas with best tracers in the lower emission corona, are accurate enough for a comparison with rotational information about another layers of the solar outer atmosphere.