  Thanks to space-borne experiments such as the AMS-02 and PAMELA missions in
low-Earth orbit, along with the Voyager spacecrafts in the interstellar space,
a large collection of multi-channel and time-resolved Galactic cosmic ray (GCR)
data has recently become available. Here we present an improved
measured-validated model of the "solar modulation" effect, i.e., the temporal
evolution of the GCR flux inside the heliosphere caused by the 11-year
variability cycle of the Sun's magnetic activity. We present our improved
modeling of the structure of the heliosphere, the physical mechanisms of
diffusion, drift, and energy losses of GCR particles in the heliosphere. We
present our results for the temporal dependence of the key model parameters and
their relationship with solar activity proxies. We discuss implications for the
GCR transport in magnetic turbulence, and new insights on our understanding of
the solar modulation phenomenon.
