Comparing pairs of successive corotating interaction regions

Coronal holes on the Sun emit solar wind at a higher speed than the areas around them. The faster streams of solar wind catch up to the slower solar wind, which was emitted before them, and compress the slower solar wind. This causes an increase in density and magnetic fields which is known as a corotating interaction region (CIR). In this study, we are primarily concerned with pairs of successive CIRs. Successive CIRs are two CIR's that are produced by the same coronal hole on the Sun and are observed on successive rotations of the Sun, where one rotation is about 27 Earth days. Once all of the CIR sets are obtained, we will compare and contrast various parameters, such as magnetic field and velocity, between the two CIRs within each set. We expect the two successive CIRs to behave in a similar manner and have similar parameters.