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Abstract
For the Schwarzschild black hole, the BekensteinHawking entropy is proportional to the area of the event horizon. For the black holes with two horizons, the thermodynamics is not very clear, since the role of the inner horizons is not well established. Here we calculate the entropy of the ReissnerNordström black hole and of the Kerr black hole, which have two horizons. For the spherically symmetric ReissnerNordström black hole, we used several different approaches. All of them give the same result for the entropy and for the corresponding temperature of the thermal Hawking radiation. The entropy is not determined by the area of the outer horizon, and it is not equal to the sum of the entropies of two horizons. It is determined by the correlations between the two horizons, due to which the total entropy of the black hole and the temperature of Hawking radiation depend only on mass M of the black hole and do not depend on the black hole charge Q. For the Kerr and KerrNewman black holes, it is shown that their entropy has the similar property: it depends only on mass M of the black hole and does not depend on the angular momentum J and charge Q.
Original language  English 

Article number  2150177 
Number of pages  12 
Journal  MODERN PHYSICS LETTERS A 
Volume  36 
Issue number  24 
DOIs  
Publication status  Published  10 Aug 2021 
MoE publication type  A1 Journal articlerefereed 
Keywords
 Black hole
 entropy
 Hawking radiation
 inner horizon
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 1 Finished

TOPVAC: From Topological Matter to Relativistic Quantum Vacuum
Volovik, G., Nissinen, J., Eltsov, V., Rysti, J., Rantanen, R., Mäkinen, J., Zhang, K., Laurila, S., Volard, M. & Kamppinen, T.
01/10/2016 → 30/09/2022
Project: EU: ERC grants