  We present observations of the extended solar cycle activity in white-light
coronagraphs, and compare them with the more familiar features seen in the Fe
XIV green-line corona. We show that the coronal activity zones seen in the
emission corona can be tracked high into the corona. The peak latitude of the
activity, which occurs near solar maximum, is found to be very similar at all
heights. But we find that the equatorward drift of the activity zones is faster
at greater heights, and that during the declining phase of the solar cycle, the
lower branch of activity (that associated with the current cycle) disappears at
about 3 Ro. This implies that that during the declining phase of the cycle, the
solar wind detected near Earth is likely to be dominated by the next cycle. The
so-called "rush to the poles" is also seen in the higher corona. In the higher
corona it is found to start at a similar time but at lower latitudes than in
the green-line corona. The structure is found to be similar to that of the
equatorward drift.
