Аннотация:Analysis of interaction between different coronal structures of solar wind (SW) sources
in the solar corona is important for improving methods of forecasting for all types of SW
streams. Several cases of considerable discrepancy between the forecasted and observed at 1
AU (spacecraft ACE) positions of recurrent SW streams in the 24th solar cycle were
analyzed. Such discrepancy can be detected in profile (in magnitude of the SW speed) and in
the arrival time of the SW stream. Possible reasons for this discrepancy related to the position
and magnetic configuration of the sources of high-speed and transient SW streams in the solar
corona were considered. It was found that deflection of high-speed SW streams produced by
high-latitude coronal holes (CHs) aside from the ecliptic plane could be caused by interaction
with transient streams originated in active regions located between CH and the solar equator.
The arrival of high-speed SW stream up to two days earlier the forecast may be associated
with the SW stream deflection to the West from the radial direction caused by interaction with
the transients whose magnetic field lines adjoining to the CH are parallel to the lines of highspeed
SW stream from the CH.