  Low energy cosmic rays are modulated by the solar activity when they
propagation in the heliosphere, leading to ambiguities in understanding their
acceleration at sources and propagation in the Milky Way. By means of the
precise measurements of the $e^-$, $e^+$, $e^-+e^+$, and $e^+/(e^-+e^+)$
spectra by AMS-02 near the Earth, as well as the very low energy measurements
of the $e^-+e^+$ fluxes by Voyager-1 far away from the Sun, we derive the local
interstellar spectra (LIS) of $e^-$ and $e^+$ components individually. Our
method is based on a non-parametric description of the LIS of $e^-$ and $e^+$
and a force-field solar modulation model. We then obtain the evolution of the
solar modulation parameters based on the derived LIS and the monthly fluxes of
cosmic ray $e^-$ and $e^+$ measured by AMS-02. {\bf To better fit the monthly
data, additional renormalization factors for $e^-$ and $e^+$ have been
multiplied to the modulated fluxes.} We find that the inferred solar modulation
parameters of positrons are in good agreement with that of cosmic ray nuclei,
and the time evolutions of the solar modulation parameters of electrons and
positrons differ after the reversal of the heliosphere magnetic field polarity,
which shows clearly the charge-sign dependent modulation effect.
