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The bright blazar OJ 287 is the best-known candidate for hosting asupermassive black hole binary system. It inspirals due to the emission ofnanohertz gravitational waves (GWs). Observations of historical and predictedquasi-periodic high-brightness flares in its century-long optical lightcurve,allow us to determine the orbital parameters associated with the binary blackhole (BBH) central engine. In contrast, the radio jet of OJ 287 has beencovered with Very Long Baseline Interferometry (VLBI) observations for onlyabout $30$ years and these observations reveal that the position angle (PA) ofthe jet exhibits temporal variations at both millimetre and centimetrewavelengths. Here we associate the observed PA variations in OJ 287 with theprecession of its radio jet. In our model, the evolution of the jet directioncan be associated either with the primary black hole (BH) spin evolution orwith the precession of the angular momentum direction of the inner region ofthe accretion disc. Our Bayesian analysis shows that the BBH central enginemodel, primarily developed from optical observations, can also broadly explainthe observed temporal variations in the radio jet of OJ 287 at frequencies of86, 43, and 15 GHz. Ongoing Global mm-VLBI Array (GMVA) observations of OJ 287have the potential to verify our predictions for the evolution of its $86$ GHzPA values. Additionally, thanks to the extremely high angular resolution thatthe Event Horizon Telescope (EHT) can provide, we explore the possibility totest our BBH model through the detection of the jet in the secondary blackhole.

Explaining temporal variations in the jet position angle of the blazar OJ 287 using its binary black hole central engine model