Co-rotating interaction region
A term used in space weather to denote a compression region ahead of a coronal hole
high-speed stream (CH HSS). They form due to the interaction of slower, ambient solar wind
ahead of the higher-speed stream. They are not associated with every CH HSS; however, they most often develop ahead of the more persistent coronal holes. They usually result in particle density
enhancement and interplanetary magnetic field strength increases and can cause geomagnetic storms
when reaching Earth.
Space Weather Prediction Center, 2018: Coronal holes. Accessed 13 August 2018. Available at https://www.swpc.noaa.gov/phenomena/coronal-holes.
Space Weather Prediction Center, 2018: Solar wind. Accessed 13 August 2018. Available at https://www.swpc.noaa.gov/phenomena/solar-wind.
Term edited 13 August 2018.