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We show the results of two dimensional general relativistic inviscid andisothermal hydrodynamical simulations comparing the behavior of co-rotating(with respect to the black hole rotation) and counter-rotating circumbinaryquasi-Keplerian discs in the post merger phase of a supermassive binary blackhole system. While confirming the spiral shock generation within the disc dueto the combined effects of mass loss and recoil velocity of the black hole, wefind that the maximum luminosity of counter-rotating discs is a factor ~(2-12)higher than in the co-rotating case, depending on the spin of the black hole.On the other hand, the luminosity peak happens ~10 days later with respect tothe co-rotating case, for a binary with a total mass M~10^6 M_\odot. Althoughthe global dynamics of counter-rotating discs in the post merger phase of amerging event is very similar to that for co-rotating discs, an importantdifference has been found. In fact, increasing the spin of the central blackhole produces more luminous co-rotating discs while less luminouscounter-rotating ones.

Electromagnetic counterparts from counter-rotating relativistic kicked discs