Prediction of the Coronal Structure for the Solar Eclipse of September 22, 1968

Abstract

A METHOD of determining the large scale structure of the coronal and interplanetary magnetic fields has recently been described¹. The model originated as an attempt to explain the observed large scale structure of the interplanetary magnetic fields. The model has been partially validated by successful comparisons of the observed interplanetery magnetic field with a field computed from photospheric observations according to this formalism. I have established further evidence in support of the model by comparisons of the computed coronal magnetic structure with coronal green line (γ5303) emission². The model has been further investigated by comparisons with the coronal structures revealed in eclipse photographs, and this process has suggested the possibility of making a prediction of the coronal structures to be expected at the solar eclipse of September 22, 1968.