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We study, by means of numerical simulations and analysis, the details of theaccretion process from a disc onto a binary system. We show that energy isdissipated at the edge of a circumbinary disc and this is associated with thetidal torque that maintains the cavity: angular momentum is transferred fromthe binary to the disc through the action of compressional shocks and viscousfriction. These shocks can be viewed as being produced by fluid elements whichdrift into the cavity and, before being accreted, are accelerated ontotrajectories that send them back to impact the disc. The rate of energydissipation is approximately equal to the product of potential energy per unitmass at the disc's inner edge and the accretion rate, estimated from the discparameters just beyond the cavity edge, that would occur without the binary.For very thin discs, the actual accretion rate onto the binary may besignificantly less. We calculate the energy emitted by a circumbinary disctaking into account energy dissipation at the inner edge and also irradiationarising there from reprocessing of light from the stars. We find that, fortight PMS binaries, the SED is dominated by emission from the inner edge atwavelengths between 1-4 and 10 $\mu$m. This may apply to systems like CoRoT223992193 and V1481 Ori.

On the energy dissipation rate at the inner edge of circumbinary discs