Abstract
Based on long-term monitoring data of the blazar, a new model for determining the parameters of this close binary supermassive black hole (SMBH) is proposed. The model uses the laws of celestial mechanics and results of harmonic analysis of observational data obtained mainly in the radio and optical wavelength ranges. Within the framework of the proposed model, the masses of SMBH companions, the values of their orbital elements, the parameters of the accretion disk, and its dimensions and thickness were determined. The structure and dynamics of SMBHs and their interaction with the accretion disk are considered. It is shown that OJ 287 may be the most massive close binary SMBH with comparable masses. The obtained characteristics of the SMBH are used to estimate the level of gravitational wave radiation, the lifetime of the system before the merger, as well as the magnitude of changes in the orbits of the companions.
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