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On 28 January 2018, the High Energy Stereoscopic System (H.E.S.S.) reported asignificant very-high-energy (VHE) gamma-ray activity, occurring nearly 11 daysafter the high-energy (HE) gamma-ray flare observed by \textit{Fermi}-LAT fromthe blazar 3C 279. It has long been considered a candidate site foraccelerating particles to ultra-high energies (UHE) and producing subsequentsecondaries. Such an event can be crucial to explore the different phenomena ofsecondary production from the UHEs and viable to understand the energetics ofthe sources. Our study finds that the multi-wavelength flare, spanning UV,optical, X-rays, and HE gamma rays, originates from leptonic emissions, whereasthe delayed VHE activity by proton synchrotron emission within the source,results from the extended duration of particle acceleration. To explain theprolonged electromagnetic emission, our model requires a magnetic fieldluminosity (L$'_B$) $6.1 \times 10^{43}$ erg/sec, a proton luminosity(L$'_{p}$) $1.2\times 10^{46}$ erg/sec in the jet frame.

Time-lag in hadronic channel: to explore delayed VHE-flare of 3C 279