  The correlation between optical and $\gamma$-ray flux variations in blazars
reveals a complex behaviour. In this study, we present our analysis of the
connection between changes in optical and $\gamma$-ray emissions in the blazar
Ton 599 over a span of approximately 15 years, from August 2008 to March 2023.
Ton 599 reached its highest flux state across the entire electromagnetic
spectrum during the second week of January 2023. To investigate the connection
between changes in optical and $\gamma$-ray flux, we have designated five
specific time periods, labeled as epochs A, B, C, D, and E. During periods B,
C, D, and E, the source exhibited optical flares, while it was in its quiescent
state during period A. The $\gamma$-ray counterparts to these optical flares
are present during periods B, C, and E, however during period D, the
$\gamma$-ray counterpart is either weak or absent. We conducted a broadband
spectral energy distribution (SED) fitting by employing a one-zone leptonic
emission model for these epochs. The SED analysis unveiled that the optical-UV
emission primarily emanated from the accretion disk in quiescent period A,
whereas synchrotron radiation from the jet dominated during periods B, C, D,
and E. Diverse correlated patterns in the variations of optical and
$\gamma$-ray emissions, like correlated optical and $\gamma$-ray flares, could
be accounted for by changes in factors such as the magnetic field, bulk Lorentz
factor, and electron density. On the other hand, an orphan optical flare could
result from increased magnetic field and bulk Lorentz factor.
