IceCube collaboration reported a ∼ 290 TeVhigh energy neutrino signal on 22 September 2017,which is usually referred to as IceCube-170922A. Thebest-fitting direction of IceCube-170922A is very closeto that of the TXS 0506+056 blazar. It means thatIceCube-170922A is consistent with the γ-ray flare of TXS 0506+056. To properly understand this phenomenon, we introduce a model involving synchrotronself-Compton and hadronic scenarios to explain the cooperative event. For the hadronic scenario, we assumethat the protons follow a power-law distribution witha high-energy cutoff under the effect of non-relativisticshock and synchrotron emission. We then consider thesynchrotron emission of protons and investigate the interaction of protons with the low-energy photons originated from the synchrotron emission. The protonphoton interaction is characterized by three main features: 1) the interaction produces Bethe-Heitler pairsand considers their synchrotron emission and inverseCompton scattering, 2) the decay of π0 produces γ-rays, 3) the production of π± is related to the presence of the muon neutrino, muon antineutrino, electron neutrino and electron antineutrino. Upon adopting the parametrization of the observed spectrum ofTXS 0506+056, we get the following results: 1) themodel is able to match the spectral energy distributionof TXS 0506+056, 2) the protons may indeed follow apower-law distribution with high-energy cutoff affectedby the shock in the jet, 3) the interaction of protonswith the low-energy photons may occur in the jet. Weargue that the high energy neutrino radiation IceCube-170922A may be understood in terms of the decay of π± produced in the interactions of protons with thesynchrotron photons in the jet, and the antineutrinosis equal to the neutrino spectrum nearly.