Emission corona and prominences over solar cycles

We present the distribution of prominences and emission coronae: Fe XIV (530.3 nm or the green corona) and Fe X (637.4 nm or the red corona), over solar cycles. There were found both polar and equatorial branches of prominences migrating in opposite directions. Similar branches were also found in the green and red corona. However, while the green corona pattern almost mimics the prominence distribution, the red corona exhibits similar behaviour in the equatorial one only. We guess that the polar prominence branches will reach the poles in 2002 (N-pole) and 2003 (S-pole), and the next solar minimum should occur in 2007. Long-term (cycle-to-cycle), medium-term (weeks or months), and shortterm changes (min or seconds) of the N-S asymmetry in both coronal lines are then discussed, together with the multiplicity, area and height of prominences.