Accretion and wind dynamics in tidal disruption events

Abstract

We have constructed self similar models of time dependent and non relativistic ac- cretion disks in both sub and super-Eddington phase of TDEs with wind outflows for a general viscosity prescription which is a function of surface density of the disk Σ d and radius r .The physical parameters are black hole (BH) mass M • , specific orbital energy E and angular mo- mentum J ,starmass M

and radius R

. We have considered an accretion disk where matter is lost due to accretion by black hole and out flowing wind (in case of super-Eddington) and added through fallback of the disrupted debris. We have simulated the light curve profiles in various spectral bands and fit them to the observations to determine the above mentioned physical parameters.