Coronal manifestations of solar variability

This contribution is mostly about phenomenology of what we see in space–time evolution of coronal green line brightness (CGLB), including its cyclic variations. Our own database (1943–2001) of the coronal Fe XIV 530.3 nm emission line intensities is used to display different aspects of the large-scale CGLB regularities and cyclic behaviour. Hemispheric asymmetry and relation of the longitudinal CGLB distribution to the rotational characteristics of the solar corona are particularly underlined.