Abstract
DURING an eclipse of the sun, changes in the electron density (N) in an ionospheric layer of Chapman type may be represented by the relation: in which q is rate of production of electrons and α′ is effective recombination coefficient. If the ionizing radiation were emitted uniformly from all parts of the disk, q would be proportional to the fraction (Ax) of the disk unobscured by the moon. Observations made at optical frequencies show that the disk radiation is not uniformly distributed. Consequently, if We assume that the ionizing radiation has a similar distribution, it is necessary to represent q during an eclipse by two terms denoting the intensity of the radiation coming from the uniform (AxI0) and non-uniform (Is) components respectively. Thus: where K is a constant and χ is zenith angle of sun.
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