  Our basic theoretical understanding of the sources of cosmic rays and their
propagation through the interstellar medium is hindered by the Sun, that
through the solar wind affects the observed cosmic-ray spectra. This effect is
known as solar modulation. Recently released cosmic-ray observations from the
Alpha Magnetic Spectrometer (AMS-02) and publicly available measurements of the
solar wind properties from the Advanced Composition Explorer and the Wilcox
observatory allow us to test the analytical modeling of the time-, charge- and
rigidity-dependence of solar modulation. We rely on associating measurements on
the local heliospheric magnetic field and the heliospheric current sheet's tilt
angle, to model the time-dependence and amplitude of cosmic-ray solar
modulation. We find evidence for the solar modulation's charge- and
rigidity-dependence during the era of solar cycle 24. Our analytic prescription
to model solar modulation can explain well the large-scale time-evolution of
positively charged cosmic-ray fluxes in the range of rigidities from 1 to 10
GV. We also find that cosmic-ray electron fluxes measured during the first
years of cycle 24 are less trivial to explain, due to the complex and rapidly
evolving structure of the Heliosphere's magnetic field that they experienced as
they propagated inwards.
