Non-Minimally Coupled Scalar Field, Area Quantization and Black Hole Entropy

Abstract

The enumeration of black hole entropy in candidate theories of quantum gravity utilises the quantum properties of microstates residing on the black hole horizon. For example, in Loop Quantum Gravity, the computation of entropy is based on the spectrum of area operator, and one determines the possible number of area mirocrostates corresponding to a given classical horizon area. In this paper, we derive the eigenspectrum of the horizon area operator for rotating/non-rotating black holes in a gravitational theory non-minimally coupled to scalar fields. Using the weak isolated horizon formalism, we show that the spectrum of area operator follows unambiguously from the algebra of horizon symmetry. More precisely, from the quantum mechanical point of view, the horizon geometry must be naturally discrete, a conclusion which is arrived at directly, without the need for any particular theory of quantum gravity. The area spectrum depends on the Barbero-Immirzi parameter as well as the value of scalar field on horizon. The area spectrum is equidistant, which is consistent with the Bekenstein-Mukhanov proposal and gives rise to black hole entropy and their quantum corrections.

Figures (1)

• Figure 1: $M_{\pm}$ are two partial Cauchy surfaces enclosing a region of space-time and intersecting $\Delta$ in the 2-spheres $S_{\pm}$ respectively,and extend to spatial infinity $i^0$. Another Cauchy slice M is drawn which intersects $\Delta$ in $S_{\Delta}$