Speaker
Description
Most galaxies harbour a super-massive black hole (SMBH) in their centre but deriving its physical properties is not straightforward, especially if it is in quiescent state. If a star falls inside the tidal radius of the black hole its disruption can set on the accretion, which produces a distinctive observational signature. However, for characterising the SMBH from the observed tidal disruption event (TDE) it is necessary to understand the physical mechanisms acting and their impact on the observational light curve. In this work, we study that the effect that general relativistic precession of the tidal stream of the disrupted star imprints on the observed light curves of tidal disruption events. We conduct moving-mesh radiation-hydrodynamic simulations of an isotropic wind and irradiation that follows the analytical TDE fallback rate interacting with the stream of the disrupted star after winding around the SMBH before triggering the event. We explore the impact of the SMBH mass, accretion efficiency parameter $\eta$, and line-of-sight angle of the event. We present first results and effects on the observed light curves.
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