Collapsar Entropy: The Choice of the Level of Description (G) and Alternative Values

This paper considers collapsar (black hole) entropy within the framework where entropy is a function of two factors: the number of accessible microstates (Ω) and the choice of the level of description (G), also called coarse‑graining. It is shown that the traditional Bekenstein–Hawking formula S = A/(4\ell_P^2) corresponds to an extreme macroscopic choice of G: only the horizon area is taken into account, while the internal structure and quantum fluctuations are “lumped together” into a single macrostate. Three alternative choices of G are analyzed: 1. Extremely macroscopic – only mass or charge is considered. Ω decreases, entropy falls. This is second‑level coarse‑graining. 2. Quantum – quantum fluctuations of the horizon are included. Ω increases, entropy rises (supported by the work of ’t Hooft and Marolf). 3. Including internal structure – everything inside the collapsar (fuzzball microstates) is taken into account. Ω becomes astronomically huge, entropy huge, but such entropy is unobservable from outside. It is concluded that “black hole entropy” is not an absolute quantity; it depends on the chosen level of description. Recognizing the role of G removes the “information paradox”: information loss is not the disappearance of a physical configuration but a consequence of the choice of G that does not include internal structure. The paper draws on modern research (Marolf, ’t Hooft, Mathur, AMPS) and is addressed to physicists and methodologists of science.