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Dark matter from quasi–de Sitter horizons

Stefano Profumo*

  • Department of Physics, University of California Santa Cruz, 1156 High Street, Santa Cruz, California 95064, USA and Santa Cruz Institute for Particle Physics, 1156 High Street, Santa Cruz, California 95064, USA

  • *Contact author: profumo@ucsc.edu
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Phys. Rev. D 112, 023511 – Published 8 July, 2025

DOI: https://doi.org/10.1103/vmw2-4k77

Abstract

Assuming that (1) the Universe underwent a postinflationary accelerated expansion phase driven by a fluid with equation of state P=wρ and −1<w<−1/3, that (2) the cosmic horizon in an accelerating, quasi–de Sitter Universe has a temperature inversely proportional to the proper size of the horizon, and that (3) we are static observers, we calculate the frozen-in density of a stable particle of mass m produced by the cosmic horizon that does not undergo any number-changing processes in the late Universe. We find that, as a function of the equation of state and the temperature when radiation domination starts and the quasi–de Sitter phase ends, the mass of the dark matter producing the observed cosmological abundance via this mechanism ranges from 10 keV up to close to the Planck scale.

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Information

Phys. Rev. D 112, 023511– Published 8 July, 2025
  • Received 28 February 2025
  • Accepted 23 June 2025
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Published by the American Physical Society under the terms of the Creative Commons Attribution 4.0 International license. Further distribution of this work must maintain attribution to the author(s) and the published article’s title, journal citation, and DOI. Funded by SCOAP3.

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