Dynamical Casimir Effect and vacuum friction in the near-horizon geometry of a black hole
Abstract
We investigate the Dynamical Casimir Effect (DCE) for a relativistic scalar field confined within a cavity possessing moving boundaries in the (1+1)-dimensional near-horizon geometry of a black hole. By applying a coordinate transformation, we map the moving-boundary problem to an equivalent acoustic metric with static boundaries, allowing for an exact canonical Hamiltonian formulation. We find that the local gravitational redshift fundamentally alters the vacuum structure, and the dynamical boundary motion induces time-dependent mode-mixing. When a boundary moves, it scatters the fluctuations of the ambient Hartle-Hawking state, generating excitations within the cavity. For sinusoidal motion, we choose a small fixed fractional amplitude and impose the timelike-wall condition. When the drive tracks the resonant sum of fixed mode numbers, the effective Mach number approaches zero as the optical length increases. At leading perturbative order and over a fixed Killing-time interval of the specified drive, the vacuum transition probability for a fixed pair scales as D 0 − 4 , where D 0 = ln ( g / f 0 ) . Furthermore, we account for the Bose-enhancement caused by the thermal Hawking bath. The net mean pair yield, after subtracting inverse absorption, scales as D 0 − 3 for the same fixed pair and driving interval. These scalings depend on the driving protocol and do not establish a universal suppression of particle creation for arbitrary timelike trajectories or for the full three-dimensional field.
Related
- Thermal vacuum friction of objects with different dimensionality
- Robustness of Dynamical Casimir Effect-Induced Quantum Synchronization
- Relativistic dynamical friction in Kerr-Schild coordinates
- Dynamical friction on black holes in scalar field environment
- Renormalized Dynamical Friction in Black-Hole Spacetimes
BibTeX
@article{hadi2026dynamical,
title = {{Dynamical Casimir Effect and vacuum friction in the near-horizon geometry of a black hole}},
author = {H. Hadi and Amin Rezaei Akbarieh and Göksel Daylan Esmer},
journal = {Physics Letters B},
year = {2026},
month = oct,
doi = {10.1016/j.physletb.2026.141080},
url = {https://linkinghub.elsevier.com/retrieve/pii/S0370269326009305},
note = {CC BY 4.0},
}
RIS
TY - JOUR
TI - Dynamical Casimir Effect and vacuum friction in the near-horizon geometry of a black hole
AU - H. Hadi
AU - Amin Rezaei Akbarieh
AU - Göksel Daylan Esmer
PY - 2026
DA - 2026/10/30
JO - Physics Letters B
DO - 10.1016/j.physletb.2026.141080
UR - https://linkinghub.elsevier.com/retrieve/pii/S0370269326009305
AB - We investigate the Dynamical Casimir Effect (DCE) for a relativistic scalar field confined within a cavity possessing moving boundaries in the (1+1)-dimensional near-horizon geometry of a black hole. By applying a coordinate transformation, we map the moving-boundary problem to an equivalent acoustic metric with static boundaries, allowing for an exact canonical Hamiltonian formulation. We find that the local gravitational redshift fundamentally alters the vacuum structure, and the dynamical boundary motion induces time-dependent mode-mixing. When a boundary moves, it scatters the fluctuations of the ambient Hartle-Hawking state, generating excitations within the cavity. For sinusoidal motion, we choose a small fixed fractional amplitude and impose the timelike-wall condition. When the drive tracks the resonant sum of fixed mode numbers, the effective Mach number approaches zero as the optical length increases. At leading perturbative order and over a fixed Killing-time interval of the specified drive, the vacuum transition probability for a fixed pair scales as D 0 − 4 , where D 0 = ln ( g / f 0 ) . Furthermore, we account for the Bose-enhancement caused by the thermal Hawking bath. The net mean pair yield, after subtracting inverse absorption, scales as D 0 − 3 for the same fixed pair and driving interval. These scalings depend on the driving protocol and do not establish a universal suppression of particle creation for arbitrary timelike trajectories or for the full three-dimensional field.
SN - 0370-2693
SN - 1873-2445
ER -