We have continuously observed muon intensities from 2000 to the present using the multidirectional
muon telescope GRAPES-3 in Ooty, South India. The radial diffusion coefficient and
the mean free path of propagation of the Galactic cosmic rays (GCR) in the heliosphere have
been derived from the density gradient obtained from the flow perpendicular to the ecliptic plane
of GCR, which depends on the polarity of the interplanetary magnetic field (IMF) (Kojima et
al., 2018). In this study, we used the data set for the years 2000-2021, covering about 8,000
days and divided into 13 groups by the solar wind velocity to examine the relationship between
the amplitude and phase of the flow as mentioned above of each group with the average solar
wind velocity on the corresponding group. This analysis shows a positive correlation between
the amplitude and phase of the flow of galactic cosmic rays perpendicular to the ecliptic plane,
depending on the polarity of the IMF and the solar wind velocity.