Long-Term Evolution of the Solar Corona Using PROBA2 Data

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/ Large Yield 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 ∘ was around 15 degree day −1 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 R ⊙ .