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tokens: BBHs in the sense that it can be detectable before the GW signal and that the luminosity increases with time. However, the luminosity and total energy are too low to explain GRBs or the GBM event (Connaughton etal. 2016 ). Figure 3. The photon fluxes from the internal shocks for models A, B and C. The 1-scan sensitivity of MAXI GSC is also plotted. It is found that all the models are detectable by MAXI GSC. The optical follow-up surveys for GW counterparts, such as the Panoramic Survey Telescope Rapid Response System (Pan-STARRS) and the Japanese collaboration for Gravitational wave ElectroMagnetic follow-up, have a sensitivity of 1921 mag (Morokuma etal. 2016 ; Smartt etal. 2016 ). Assuming that 10percent of L AG is in the optical range, we calculate the distance of detection limit for the afterglow, d L, lim , whose values are tabulated in Table 1 . While the afterglow is fainter than the internal shock emission, the optical follow-up surveys of afterglows can detect comparable or more distant events than the X-ray monitoring systems owing to the good sensitivity. However, d L, lim for model A is shorter than the distance of the observed GW events (Abbott etal. 2016a , b ). Although d L, lim is larger for IMBHs and MBHs, we do not discuss the detection probability because the merger rates of IMBH and MBH binaries are very uncertain. 4 SUMMARY and DISCUSSION We study evolution of an accretion disc in BBH systems and propose an evolutionary track of the disc, which leads to different conclusion from the previous work (Perna etal. 2016 ). At first, the disc viscously expands outward but the companion prevents the disc from expanding beyond r out due to the tidal torque. The evolution of viscous disc results in the decrease of the disc mass and the temperature. When the disc sufficiently cools down (typically less than 3000K), the dead disc forms because MRI becomes inactive. Since the thermal instability causes the rapid drop of the disc temperature, the disc becomes dead when the temperature becomes less than a few tens of thousands K. This dead disc remains until the binary separation sufficiently decreases. As the binary separation decreases, the position at which the tidal torque is effective moves inward, and the mass of the outer rim increases. Then, the angular momentum is transported by the tidal torque, which induces the mass inflow from the outer rim to the dead disc. When the mass inflow by the tidal torque becomes higher than , the accretion heating activates MRI, restarting the mass accretion from the disc to the central BH (the disc revival). This disc revival typically happens tens of thousands years before the merger event. The evolution of the revival disc is determined by the tidal torque, keeping t vis t GW . The mass accretion rate of the revival disc increases with time. In the late phase of the revival disc evolution, the mass accretion rate can exceed Eddington rate, and a relativistic jet is expected to be