How the area of solar coronal holes affects the properties of high-speed solar wind streams near Earth: An analytical model

Since the 1970s it has been empirically known that area of solar coronal holes affects properties high-speed wind streams (HSSs) at Earth. We derive a simple analytical model for propagation HSSs from Sun to Earth and thereby show how size their boundary regions affect HSS velocity, temperature, density near assume profiles form across cross section close these spatial translate into corresponding temporal in given radial direction due rotation. These distributions drive stream interface preceding slow plasma disperse with distance Sun. The 1 AU are then by all parcels launched did not run distance. velocity plateau region as seen AU, if apparent, originates center Sun, whereas tail trailing region. Small can be described entirely consist plasma, which intrinsically results smaller peak velocities. further depends on longitudinal width shorter an more its “fastest” core have impinged upon wind, is As statistically correlated holes, this also explains well-known empirical relationship between hole areas Further, temperature depend expansion determined gradient gives velocity-temperature density-temperature relationships specific shape. When considering large number HSSs, assumed correlation velocities temperatures degrades only slightly up but densities strongly disrupted expansion. Finally, we particles piled-up interaction plasma.