Abstract An analysis is made of variations in length of quiescent solar filaments and of solar wind parameters. The study revealed some peculiarities of annual and quasi-biennial variations of these characteristics; in particular, it was found that in March–April of the odd years there is a significant increase in the number of days occupied by high speed streams, which triggers a substantial enhancement of geomagnetic activity. It is shown that the dynamics of large-scale solar magnetic fields are quite well manifested in the particle flux density of the solar wind for different velocity regimes and the occurrence frequency of high ( V > 500 km s −1) and low ( V < 400 km s −1) solar wind velocities. We discuss the possible changes of solar magnetic fields which could be responsible for the observed variations of these parameters. We analyse, in terms of a solar wind formation model developed by the present authors, the relationship between the variability of large-scale solar magnetic fields and properties of the solar wind for its different formation regimes.