  In the binary black hole model of OJ 287 the secondary black hole orbits a
much more massive primary, and impacts on the primary accretion disk at
predictable times. We update the parameters of the disk, the viscosity $\alpha$
and the mass accretion rate $\dot m$. We find $\alpha=0.26 \pm 0.1$ and $\dot m
= 0.08 \pm 0.04$ in Eddington units. The former value is consistent with
Coroniti (1981) and the latter with Marscher and Jorstad (2011). Predictions
are made for the 2019 July 30 superflare in OJ 287. We expect that it will take
place simultaneously at the Spitzer infrared channels as well as in the optical
and that therefore the timing of the flare in optical can be accurately
determined from Spitzer observations. We also discuss in detail the light curve
of the 2015 flare and find that the radiating volume has regions where
bremsstrahlung dominates as well as regions that radiate primarily in
synchrotron radiation. The former region produces the unpolarised first flare
while the latter region gives rise to a highly polarized second flare.
