Area Spectrum and Black Hole Thermodynamics

The role of horizon area quantization in black hole (BH) thermodynamics is investigated. The coefficient appearing in the quantization of area is fixed by an appeal to the saturated form of Landauer’s principle. Then, by considering a transition between discrete states of the event horizon area, which is in turn equivalent to transitions between discrete mass states of the BH, the change in mass can be obtained. The change in mass is then equated to a product of the Hawking temperature and the change in BH entropy between two consecutive discrete states, applying the first law of BH thermodynamics. This gives the corrected Hawking temperature. In particular, we apply this technique to the Schwarzschild BH, the quantum corrected Schwarzschild BH, the Reissner–Nordström charged BH, and the Kerr rotating Kerr BH geometry, and obtain a corrected Hawking temperature in each of these cases. We then take a step forward by inserting this corrected Hawking temperature in the first law of BH thermodynamics once again to calculate the BH entropy in terms of the BH horizon area. This leads to logarithmic and inverse corrections to the BH entropy.