Dynamical Tsallis WIMP Freeze-Out and Residual Memory Channels in the Radiation Sector
Abstract
In this work we generalize the thermal decoupling, or freeze-out, of weakly interacting massive particle dark matter within the Tsallis nonextensive formalism. The generalization is implemented through q-deformed distribution functions obtained from the maximum entropy principle with Curado-Tsallis constraints. The Tsallis parameter q, which measures deviations from extensivity with respect to the limit q=1, is promoted to a dynamical quantity depending on the dimensionless variable x=mχ/T, where mχ is the dark matter mass. This dynamical evolution is characterized by a relaxation toward extensivity, while requiring that the nonextensive deformation is not completely erased before freeze-out. We solve the Boltzmann equation assuming a sectorial deformation, where only the dark matter equilibrium abundance is generalized and the radiation background remains extensive. The relic abundance is computed for different dark matter masses and initial values of the Tsallis parameter. From this evolution, we extract the residual value qχfo at freeze-out, which is then used as the initial input for a phenomenological memory channel. This channel propagates the residual nonextensivity into the radiation sector, specifically into the electron-positron plasma and neutrinos, while photons are kept extensive in order to avoid direct tensions with CMB physics. The resulting deformation modifies the neutrino energy density and the photon reheating contribution, producing a correction to Neff. We compare the predicted values with the compressed CMB+BAO constraint on Neff and find that the residual-memory scenario can remain phenomenologically compatible with current bounds.
Related
- Graceful Exit to Radiation Domination in the Starobinsky Model: A Dynamical Realization
- Resolving Galactic and Cluster Dynamics Without Dark Matter: Tsallis Entropy as the Unique Foundation of Emergent Gravity
- Phantom-Divide Crossing in Barrow-Tsallis Holographic Dark Energy with a Scale-Dependent Barrow Exponent
- New Tsallis holographic dark energy with the Granda-Oliveros cutoff in a non-flat universe: curvature tracking and DESI DR2 constraints
- Kaon Portal to Freeze-in Dark Matter
BibTeX
@misc{gonzalez2026dynamical,
title = {{Dynamical Tsallis WIMP Freeze-Out and Residual Memory Channels in the Radiation Sector}},
author = {Matias P. Gonzalez},
howpublished = {arXiv},
year = {2026},
month = sep,
doi = {10.48550/arxiv.2605.29132},
eprint = {2605.29132},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2605.29132},
}
RIS
TY - UNPB
TI - Dynamical Tsallis WIMP Freeze-Out and Residual Memory Channels in the Radiation Sector
AU - Matias P. Gonzalez
PY - 2026
DA - 2026/09/09
PB - arXiv
DO - 10.48550/arxiv.2605.29132
UR - https://arxiv.org/abs/2605.29132
AB - In this work we generalize the thermal decoupling, or freeze-out, of weakly interacting massive particle dark matter within the Tsallis nonextensive formalism. The generalization is implemented through q-deformed distribution functions obtained from the maximum entropy principle with Curado-Tsallis constraints. The Tsallis parameter q, which measures deviations from extensivity with respect to the limit q=1, is promoted to a dynamical quantity depending on the dimensionless variable x=m_χ/T, where m_χ is the dark matter mass. This dynamical evolution is characterized by a relaxation toward extensivity, while requiring that the nonextensive deformation is not completely erased before freeze-out. We solve the Boltzmann equation assuming a sectorial deformation, where only the dark matter equilibrium abundance is generalized and the radiation background remains extensive. The relic abundance is computed for different dark matter masses and initial values of the Tsallis parameter. From this evolution, we extract the residual value q_χ^fo at freeze-out, which is then used as the initial input for a phenomenological memory channel. This channel propagates the residual nonextensivity into the radiation sector, specifically into the electron-positron plasma and neutrinos, while photons are kept extensive in order to avoid direct tensions with CMB physics. The resulting deformation modifies the neutrino energy density and the photon reheating contribution, producing a correction to N_eff. We compare the predicted values with the compressed CMB+BAO constraint on N_eff and find that the residual-memory scenario can remain phenomenologically compatible with current bounds.
ER -