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This work is a continuation of our previous paper [Yermolaevetal2015] whichdescribes the average temporal profiles of interplanetary plasma and fieldparameters in large-scale solar-wind (SW) streams: CIR, ICME (both MC andEjecta) and Sheath as well as the interplanetary shock (IS). Like in theprevious work we use data of OMNI database, our catalog of large-scalesolar-wind phenomena during 1976--2000 [Yermolaevetal2009] and the doublesuperposed epoch analysis (DSEA) method [Yermolaevetal2010]: re-scaling theduration of interval for all types in such a manner that, respectively,beginning and end for all intervals of selected type coincide. We present newdetailed results of comparison of two pair phenomena: (1) both types ofcompression regions (CIR.vs.Sheath) and (2) both types of ICMEs (MC.vs.Ejecta).Obtained data allows us to suggest that the formation of all types ofcompression regions has the same physical mechanism irrespective of piston(High-Speed Stream (HSS) or ICME) type and differences are connected withgeometry (angle between speed gradient in front of piston and satellitetrajectory) and full jumps of speed in edges of compression regions. One ofconsequences of this hypothesis is the conclusion that one of the reasons ofobserved distinctions of parameters in MC and Ejecta can be fact that atmeasurements of Ejecta the satellite passes further from the nose area of ICME,than at measurements of MC. We also discuss the impact of Sheath inmagnetospheric activity and its contribution in estimation of Sun's openmagnetic flux.

Dynamics of large-scale solar-wind streams obtained by the double superposed epoch analysis. 2. CIR.vs.Sheath and MC.vs.Ejecta comparisons