Abstract
By solving the field equation in curved spacetime, we obtained the relative emissivity of the Kerr–Newman black hole. The results show that the relative emissivity satisfies the Boltzmann distribution law. With the first law of thermodynamics, we found that the emissivity is related to the entropy change of black holes which helps us solve the information loss in the Hawking radiation. Through calculating the information entropy of black holes, it is shown that the information conservation is satisfied in the Hawking radiation. Furthermore, we also studied the contribution of space-time background to Hawking radiation.
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