Super-resonant dark matter at O(100) GeV masses amplifies self-scattering and annihilation cross sections via combined resonance and Sommerfeld effects, necessitating coupled Boltzmann equations to match observed relic density.
Particle Models and the Small-Scale Structure of Dark Matter
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abstract
The kinetic decoupling of weakly interacting massive particles (WIMPs) in the early universe sets a scale that can directly be translated into a small-scale cutoff in the spectrum of matter density fluctuations. The formalism presented here allows a precise description of the decoupling process and thus the determination of this scale to a high accuracy from the details of the underlying WIMP microphysics. With decoupling temperatures of several MeV to a few GeV, the smallest protohalos to be formed range between 10^{-11} and almost 10^{-3} solar masses -- a somewhat smaller range than what was found earlier using order-of-magnitude estimates for the decoupling temperature; for a given WIMP model, the actual cutoff mass is typically about a factor of 10 greater than derived in that way, though in some cases the difference may be as large as a factor of several 100. Observational consequences and prospects to probe this small-scale cutoff, which would provide a fascinating new window into the particle nature of dark matter, are discussed
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Gamma-ray upper limits from five high-energy observatories constrain the annihilation cross sections of composite dark matter in the mass range 10^5--10^12 GeV.
Filtering unidentified Fermi sources and comparing to repopulated VL-II simulations yields upper limits of 4e-26 cm3/s (10 GeV) and 5e-25 cm3/s (100 GeV) on tau-pair annihilation.
CMB data limits the s-wave annihilation cross section of thermal dark matter particles to ≲ 10^{-30} cm³/s scaled by PBH fraction and mass for PBHs heavier than ~10^{-10} solar masses.
citing papers explorer
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Self-Interaction of Super-Resonant Dark Matter
Super-resonant dark matter at O(100) GeV masses amplifies self-scattering and annihilation cross sections via combined resonance and Sommerfeld effects, necessitating coupled Boltzmann equations to match observed relic density.
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Too Heavy to Hide: Gamma-Ray Constraints on Annihilating Dark Matter beyond Unitarity
Gamma-ray upper limits from five high-energy observatories constrain the annihilation cross sections of composite dark matter in the mass range 10^5--10^12 GeV.
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Unidentified Gamma-ray Sources as Targets for Indirect Dark Matter Detection with the Fermi-Large Area Telescope
Filtering unidentified Fermi sources and comparing to repopulated VL-II simulations yields upper limits of 4e-26 cm3/s (10 GeV) and 5e-25 cm3/s (100 GeV) on tau-pair annihilation.
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In-depth analysis of the clustering of dark matter particles around primordial black holes. Part III: CMB constraints
CMB data limits the s-wave annihilation cross section of thermal dark matter particles to ≲ 10^{-30} cm³/s scaled by PBH fraction and mass for PBHs heavier than ~10^{-10} solar masses.