The bounded discrete thermal weight suppresses black-hole Hawking luminosity near the cutoff and supports an exact Jarzynski identity for work but not a simple Crooks relation.
( 15) similarly gives ∆ ⟨k⟩eff = − 1 2 bβε 2 nP (nP + 1) + O(b2), (A4) since eβε / (eβε − 1)2 = nP (nP + 1)
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Bounded thermal weights from a discrete Boltzmann factor
The bounded discrete thermal weight suppresses black-hole Hawking luminosity near the cutoff and supports an exact Jarzynski identity for work but not a simple Crooks relation.