I will present a family of spherical charged black holes in cosmological backgrounds which are solutions to an effective Hamiltonian with holonomy corrections motivated by loop quantum gravity.
Blackboard talk
In this talk, I will construct new BMS charges which are able to measure some local energy flux on the celestial sphere. For this, I will introduce an edge mode, the supertranslation field, that has already been encountered in the literature. I will show that the new charges represent the BMS group, are covariant and independent on any choice of background structure, i.e choice of foliation or conformal factor. Furthermore, there is no cocycle or central extension in the representation of the algebra. I will check that these charges have all the properties required for an asymptotic notion of (local) energy on the celestial sphere.
After introducing the main ideas behind light-cone thermodynamics, I will explicitly express the Minkowski vacuum of a massless scalar field in terms of the particle notion associated with suitable spherical conformal killing fields. These fields are orthogonal to the light wavefronts originating from a sphere with a radius of rH in flat spacetime: a bifurcate conformal killing horizon that exhibits semiclassical features similar to those of black hole horizons and Cauchy horizons of non-extremal spherically symmetric black holes. Our result highlights the quantum aspects of this analogy and extends the well-known decomposition of the Minkowski vacuum in terms of Rindler modes, which are associated with the boost Killing field normal to a pair of null planes in Minkowski spacetime (the basis of the Unruh effect).
On the one hand it is possible to determine graviton corrections to Newton's potential by treating GR as an effective field theory. On the other hand there are a multitude of quantum black hole models written as modifications of the Schwarzschild metric. I will show how it is possible to use these metrics to determine corrections to Newton's potential. I will show that in the case of the Hayward metric the corrections do not correspond to the graviton ones. Finally, I will present a generic method for testing whether a modified metric reproduces the graviton corrections to Newton's potential.