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tokens: may favour jet production. If a jet is launched, it is likely to dominate the power output of the event if viewed on-axis, where the radiation will likely be non-thermal, whereas off-axis emission is likely to be thermal. There is also the possibility of radiatively driven winds originating from the accretion disc, but we do not consider these here. Following MacLeod et al. ( 2014 ), if t visc > t fb , no longer traces , with viscous expansion of the disc modifying accretion time-scales according to (Cannizzo Gehrels 2009 ; Cannizzo, Troja Lodato 2011 ): where and α = 0.1 for thick discs. The form of during its rise is currently not well constrained; we model it crudely here using a half-Gaussian centred on t peak with σ = t peak /4, and normalize its peak to L Edd . In this work, we assume that the observable X-ray light curve will trace and plot examples of our simulated light curves following the above description in Fig. 1 . Figure 1. Simulated light curves for WTDEs based on the theory described in Section 2.1 . Higher M bh have faster rises to peak L , with fastest decay rates in light curve for BHs. For comparison of peak luminosities of these events, we normalize each light curve by L 5, peak , the Eddington luminosity of a BH. The WF experiences extreme compression perpendicular to the orbital plane, with this being maximized as it crosses pericenter. This is expected to trigger thermonuclear burning if its time-scale is much shorter than the dynamical time-scale (see eg. Luminet Pichon 1989a ; Brassart Luminet 2008 ; Rosswog et al. 2009 ; Haas et al. 2012 ). This burning originates in the tidal debris, with emission likely resembling type 1a SNe-like light curves in the optical band (Rosswog et al. 2008 , 2009 ; MacLeod et al. 2016 ; Kawana et al. 2018 ). Whilst thermonuclear burning may affect the amount of bound debris and subsequent accretion rate, no robust models of this currently exist and we neglect its impact in this work. 2.1.2 Spectral properties Following the modelling of emission from thick accretion discs (see Balbus Hawley 1998 for a review), the innermost sections of the disc, R 5 R S (as in Ulmer 1999 and Khabibullin et al. 2014 ), radiate as a blackbody at temperature: where L Edd is the Eddington luminosity of the BH. For IMBHs with masses of , this results in X-ray spectra with temperatures 0.2 keV. The soft emission from these events can be significantly affected by the interstellar medium’s (ISM’s) absorption along the line of sight (Auchettl, Guillochon Ramirez-Ruiz 2017 ). For each TDE, we set the Galactic neutral hydrogen column density, N H , to , close to the estimated extra-galactic median of N H (Esquej et al. 2008 ). We model the WTDE’s spectrum using the xspec model tbabs(zbbody) , but neglect modelling any spectral evolution. An optically thick extended envelope may form from stellar debris around the BH, reprocessing a fraction of the X-ray accretion flare into the UV and optical bands (eg. Loeb