  NH$_{3}$(ammonia) plays a critical role in the chemistry of star and planet
formation, yet uncertainties in its binding energy (BE) values complicate
accurate estimates of its abundances. Recent research suggests a multi-binding
energy approach, challenging the previous single-value notion. In this work, we
use different values of NH$_{3}$ binding energy to examine its effects on the
NH$_{3}$ abundances and, consequently, in the early evolution of protostellar
cores. Using a gas-grain chemical network, we systematically vary the values of
NH$_{3}$ binding energies in a model Class 0 protostellar core and study the
effects of these binding energies on the NH$_{3}$ abundances. Our simulations
indicate that abundance profiles of NH$_{3}$ are highly sensitive to the
binding energy used, particularly in the warmer inner regions of the core.
Higher binding energies lead to lower gas-phase NH$_{3}$ abundances, while
lower values of binding energy have the opposite effect. Furthermore, this
BE-dependent abundance variation of NH$_{3}$ significantly affects the
formation pathways and abundances of key species such as HNC, HCN, and CN. Our
tests also reveal that the size variation of the emitting region due to binding
energy becomes discernible only with beam sizes of 10 arcsec or less. These
findings underscore the importance of considering a range of binding energies
in astrochemical models and highlight the need for higher resolution
observations to better understand the subtleties of molecular cloud chemistry
and star formation processes.
