Prof. S. Shankaranarayanan

One of the most remarkable features of black hole physics is the realization that black holes behave as thermodynamic systems and possess entropy and temperature. However, black hole thermodynamics now has the problem of Universality --- at the leading order, several approaches using completely different microscopic degrees of freedom lead to Bekenstein-Hawking entropy. Currently, it is not possible to identify which are the true degrees of freedom that are responsible for the black hole entropy. Therefore other tests of reproducing black hole physics are key in distinguishing such models. In this talk, I will show that quantum entanglement of quantum fields across the black hole horizon leads to Smarr-formula of black hole thermodynamics for asymptotically flat and non-flat space-times.