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tokens: a population of stars is present, and some studies suggest they may be somewhat common (Lauer et al. 2005 ) – further increases the TDE rate. 4.4 Other sources of emission: winds and accretion on to the primary From Fig. 1 , we see that accretion on to the secondary often proceeds at a super-Eddington rate. While most of the time the rate is only mildly super-Eddington, satisfying with N ≃ few, in some cases, and particularly towards the peak in the accretion rate, N can approach and even exceed 100. While these hyper-Eddington periods are predicted analytically (Rees 1988 ; Evans Kochanek 1989 ), the peak accretion rates in Fig. 1 can actually exceed the analytical one (shown by the dashed curve in the top-left panel in this figure), which is a consequence of self-gravity (Coughlin Nixon 2015 ) and the non-zero energy of the stellar centre of mass. In these highly supercritical regimes, one might expect winds (Strubbe Quataert 2009 ; Metzger Stone 2016 ) or, in the more extreme cases, jets (Giannios Metzger 2011 ; Coughlin Begelman 2014 ; Tchekhovskoy et al. 2014 ; Coughlin Begelman 2015 ) to be launched from the vicinity of the accreting SMBH. From these outflows one would expect an additional source of radiation, with properties distinct from the disc. While it is unlikely that this scenario explains the rebrightening seen in ASASSN-15lh – the accretion rate would have been super-Eddington prior to the increase, and the constancy of the X-ray emission (Margutti et al. 2017 ) suggests that there was no change in the source of harder photons – changes in the luminosity induced by a sudden super-Eddington surge of accretion would be possible in other systems. The disk feeding the SMBH should also become geometrically thicker once the Eddington limit is surpassed, and could perhaps inflate to a quasi-spherical envelope once L ≫ L Edd (Loeb Ulmer 1997 ; Coughlin Begelman 2014 ). The simulations performed here would not capture the important physical interactions between the radiation and the plasma that would lead to such an inflated disc structure (see Sa̧dowski et al. 2016 , who do find quasi-spherical envelopes from their simulations of TDEs). Nevertheless, if the photosphere of the disk coincides with the photon trapping radius (Begelman 1979 ), then we can estimate the size of the envelope as (equation 17 of Coughlin Begelman 2014 ) where in the final line we set the opacity equal to the value for electron scattering, κ = κ es = 0.34 g cm −2 . Interestingly, this radius is of the order of the Hill sphere of the secondary for the binaries considered here; thus, the discs from super-Eddington TDEs in tight binaries could fill their Roche Lobes, resulting in accretion on to the primary. This accretion would then provide an additional source of radiation, and it would also modify the structure of the envelope around the secondary and, conceivably, its accretion rate. While it did not occur in any of our simulations, one can also imagine