  We use The Sun Watcher with Active Pixel System detector and Image Processing
(SWAP) imager onboard the Project for Onboard Autonomy 2 (PROBA2) mission to
study the evolution of large-scale EUV structures in the solar corona observed
throughout Solar Cycle 24 (from 2010 to 2019). We discuss the evolution of the
on-disk coronal features and at different heights above the solar surface based
on EUV intensity changes. We also look at the evolution of the corona in
equatorial and polar regions and compare them at different phases of the solar
cycle, as well as with sunspot number evolution and with the PROBA2/Lyman-Alpha
Radiometer (LYRA) signal. The main results are as follows: The three time
series (SWAP on-disk average brightness, sunspot number and LYRA irradiance)
are very well correlated, with correlation coefficients around 0.9. The average
rotation rate of bright features at latitudes of +15, 0, and -15 degrees was
around 15 degree/day throughout the period studied. A secondary peak in EUV
averaged intensity at the Poles was observed on the descending phase of SC24.
These peaks (at North and South poles respectively) seem to be associated with
the start of the development of the (polar) coronal holes. Large-scale off-limb
structures were visible from around March 2010 to around March 2016, meaning
that they were absent at the minimum phase of solar activity. A fan at the
North pole persisted for more than 11 Carrington rotations (February 2014 to
March 2015), and it could be seen up to altitudes of 1.6 Rs.
