For Schwarzschild black holes, generalized non-extensive entropies such as Rényi, Tsallis, and four- and five-parameter forms cannot reproduce both the Hawking temperature and the ADM mass; only the Bekenstein-Hawking entropy satisfies both.
Searching for dynamical black holes in various theories of gravity
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We construct models of Einstein and $f(R)$ gravity with two scalar fields, which admit analytical solutions describing time-varying dynamical black holes. Their thermodynamics is investigated in the adiabatic approximation. In addition to the Misner-Sharp-Hernandez quasilocal mass, we provide time-dependent thermodynamical quantities, including the Hawking temperature, Helmholtz free energy, entropy, and thermodynamical energy. The latter does not always coincide with the Misner-Sharp-Hernandez mass at the horizon, although they coincide in the static limit. For Schwarzschild-type (i.e., $g_{tt}g_{rr}=-1$) black holes in Einstein gravity, one of the two scalars is always a ghost with negative kinetic energy. We show that this ghost can be avoided in $f(R)$ gravity.
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Black Holes Thermodynamics and Generalised Non-Extensive Entropy
For Schwarzschild black holes, generalized non-extensive entropies such as Rényi, Tsallis, and four- and five-parameter forms cannot reproduce both the Hawking temperature and the ADM mass; only the Bekenstein-Hawking entropy satisfies both.