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.