Physics of tidal disruption events around black holes

In tidal disruption events (TDEs) the black hole’s tidal gravity disrupts the star and the debris accretes on to the hole. The theory of this phenomenon involves the study of dynamics of stars in the galactic center of the quiescent galaxies. The stellar dynamics of ingestion and gas dynamics of accretion in TDEs are constructed using the physical parameters such as black hole (BH) mass M•, specific orbital energy E and angular momentum J, star mass M? and radius R?, and the pericenter of the star orbit rp (E, J, M•). We constructed a stellar dynamical model using the steady loss cone formalism to estimate the theoretical capture rate of stars to be N ̇ t ∼ 10−4M−0.3 • yr−1 and a gas dynamical model for the accretion, wind, and fallback of the disrupted debris. Using the steady accretion model, instrument parameters and ΛCDM cosmology, we have calculated the detection rate of TDEs for various all-sky survey and deep imaging survey missions. The time-dependent and self-similar models of accretion disk for both the sub and super-Eddington phases evolve due to mass loss by accretion onto the black hole and an outflowing wind, and mass gain by fallback of the debris. The fit of the simulated light curves to 16 TDE observations show that the TDEs are dominated by low mass SMBHs and low mass stars. The TDEs can also be used to derive the black hole mass function (BHMF); we have calculated the Schechter BHMF parameters by comparing the expected detection rate to the observed detection rate for the various survey. The current challenges associated with TDEs and their observations through the ground and space-based detectors will also be discussed.