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Description
Tidal Disruption Events (TDEs) occur when a star gets too close to a black hole, and its gravitational pull tears the star apart. These events result in a bright burst of electromagnetic radiation and provide important information about the black hole’s environment. When the star is disrupted, approximately half of its material forms an accretion disk around the black hole. The event is mostly detected in the optical bands, although the accretion disk’s radiation lies in the X-ray regime. This phenomenon is still a subject of debate. With the Legacy Survey of Space and Time (LSST) expected to discover a vast number of new TDEs; therefore, an accurate theoretical description of these events is essential.
One of the explanations, the so-called slim disk model, states that when the fallback rate of the material exceeds the Eddington limit, a super-Eddington wind is released from the surface of the disk. The disk can sustain stability in the long term, because internal inhomogeneities reduce the effective opacity, keeping it locally sub-Eddington. The wind is optically thick, absorbing the radiation of the disk and re-emitting it at longer wavelengths.
An analytical model of TDEs based on aforementioned theory introduces a parameter describing the ratio of the wind to the disk material. The parameter largely affects the light curve of the event; therefore, its fine-tuning is crucial.
To achieve this, we present an implementation of the stationary super-Eddington slim disk model calculated for a wide parameter range of outer accretion rates and black hole accretion efficiency. This model can follow the evolution of the fallback-accretion rate and light curves of the TDEs more precisely. We used the so-called TiDE code to calculate monochromatic light curves of TDEs with our results. These light curves are compared to calculations with the old prescriptions, as well as with observations. These results demonstrate a physically consistent connection between the disk and the wind, providing an improved framework for fitting light curves of TDEs.