  Spectroscopic equilibrium allows us to obtain precise stellar parameters in
Sun-like stars. It relies on the assumption of the iron excitation and
ionization equilibrium. However, several works suggest that magnetic activity
may affect chemical abundances of young active stars, calling into question the
validity of this widely-used method. We have tested for the first time
variations in stellar parameters and chemical abundances for the young solar
twin HIP 36515 ($\sim$0.4 Gyr), along its activity cycle. This star has stellar
parameters very well established in the literature and we estimated its
activity cycle in $\sim$6 years. Using HARPS spectra with high resolving power
(115 000) and signal-to-noise ratio ($\sim$270), the stellar parameters of six
different epochs in the cycle were estimated. We found that the stellar
activity is strongly correlated with the effective temperature, metallicity,
and microturbulence velocity. The possibility of changes in the Li I 6707.8 \AA
line due to flares and star spots was also investigated. Although the core of
the line profile shows some variations with the stellar cycle, it is
compensated by changes in the effective temperature, resulting in a non
variation of the Li abundance.
