  Blazars are known to emit exceptionally variable non-thermal emission over
the wide range (from radio to $\gamma$-rays) of electromagnetic spectrum. We
present here the results of our $\gamma$-ray flux and spectral variability
study of the blazar Ton 599, which has been recently observed in the
$\gamma$-ray flaring state. Using 0.1$-$300 GeV $\gamma$-ray data from the
$\it{Fermi}$ Gamma-ray Space Telescope (hereinafter $\it{Fermi}$), we generated
one-day binned light curve of Ton 599 for a period of about one-year from MJD
59,093 to MJD 59,457. During this one year period, the maximum $\gamma$-ray
flux detected was 2.24 $\pm$ 0.25 $\times$ $10^{-6}$ ph cm$^{-2}$ s$^{-1}$ at
MJD 59,399.50. We identified three different flux states, namely, epoch A
(quiescent), epoch B (pre-flare) and epoch C (main-flare). For each epoch, we
calculated the $\gamma$-ray flux variability amplitude (F$_{var}$) and found
that the source showed largest flux variations in epoch C with F$_{var} \sim$
35%. We modelled the $\gamma$-ray spectra for each epoch and found that the
Log-parabola model adequately describes the $\gamma$-ray spectra for all the
three epochs. We estimated the size of the $\gamma$-ray emitting region as 1.03
$\times$ $10^{16}$ cm and determined that the origin of $\gamma$-ray radiation,
during the main-flare, could be outside of the broad line region.
