Stellar gravitational heating reduces dark matter spike overdensities by 2-4 orders of magnitude and drives the inner slope to γ_χ ≈ 1.5 within a few Gyrs, remaining above NFW cusps.
Road through darkνess: Probing dark matter–neutrino interactions using KM3-230213A
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IceCube diffuse neutrino data constrains neutrino loss from new physics via energy conservation, yielding bounds that vary with attenuation energy dependence and source redshift assumptions while potentially affecting spectral index fits.
Current constraints on μ-τ SMEFT four-lepton operators exclude heavy-mediator UV completions of strong neutrino self-interactions in the dimension-six SMEFT without tuned cancellations, while leaving light-mediator scenarios open.
UHE neutrino flux is attenuated by DM scatterings in intergalactic and galactic media, enabling cross-section limits from events like KM3230213A under mild astrophysical assumptions.
citing papers explorer
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Formation and Redshift Evolution of Dark Matter Spikes
Stellar gravitational heating reduces dark matter spike overdensities by 2-4 orders of magnitude and drives the inner slope to γ_χ ≈ 1.5 within a few Gyrs, remaining above NFW cusps.
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Exploring neutrino loss with diffuse astrophysical neutrino fluxes
IceCube diffuse neutrino data constrains neutrino loss from new physics via energy conservation, yielding bounds that vary with attenuation energy dependence and source redshift assumptions while potentially affecting spectral index fits.
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Theoretical and Experimental Constraints in the $\mu$--$\tau$ Four-Lepton Sector of the SMEFT: implications to neutrino self interactions
Current constraints on μ-τ SMEFT four-lepton operators exclude heavy-mediator UV completions of strong neutrino self-interactions in the dimension-six SMEFT without tuned cancellations, while leaving light-mediator scenarios open.
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Attenuation of the ultra-high-energy neutrino flux by dark matter scatterings
UHE neutrino flux is attenuated by DM scatterings in intergalactic and galactic media, enabling cross-section limits from events like KM3230213A under mild astrophysical assumptions.