SUPERMASSIVE BINARY BLACK HOLES - POSSIBLE OBSERVATIONAL EFFECTS IN THE X-RAY EMISSION

Abstract

Here we discuss the possible observational effects in the X-ray emission from two relativistic accretion disks in a supermassive binary black hole system. For that purpose we developed a model and performed numerical simulations of the X-ray radiation from a relativistic accretion disk around a supermassive black hole, based on the ray-tracing method in the Kerr metric, and applied it to the case of the close binary supermassive black holes. Our results indicate that the broad Fe K line is a powerful tool for detecting such systems and studying their properties. The most favorable candidates for observational studies are the supermassive binary black holesin the galactic mergers during the phase when the orbital velocities of their components are very large and exceed several thousand kms-1.