2023MNRAS.519.5828M

We perform a comprehensive analysis of a population of 19 X-ray bright tidal disruption events (TDEs), fitting their X-ray spectra with a new, physically self-consistent, relativistic accretion disc model. Not all of the TDEs inhabit regions of parameter space where the model is valid, or have sufficient data for a detailed analysis, and physically interpretable parameters for a subsample of 11 TDEs are determined. These sources have thermal (power-law free) X-ray spectra. The radial sizes measured from these spectra lie at values consistent with the innermost stable circular orbit of black holes with masses given by the M_BH-σ relationship, and can be used as an independent measurement of M_BH. The bolometric disc luminosity can also be inferred from X-ray data. All of the TDEs have luminosities that are sub-Eddington (L_bol, disc_ ≲ L_edd), and larger than the typical hard-state transitional luminosity of X-ray binary discs (L_bol, disc_ ≳ 0.01L_edd). The peak bolometric luminosity is found to be linearly correlated with the M_BH-σ mass. The TDE X-ray-to-bolometric correction can reach values up to ∼100, and grows exponentially at late times, resolving the missing energy problem. We show that the peak disc luminosities of some TDEs are smaller than their observed optical luminosities, implying that not all of the early time optical emission can be sourced from reprocessed disc emission. Our results are supportive of the hypothesis that thermal X-ray bright TDEs are in accretion states analogous to the 'soft' accretion state of X-ray binaries, and that black hole accretion processes are scale (mass) invariant.