Solar-reflected inelastic dark matter produces detectable signals in xenon and semiconductor detectors, enabling new constraints on MeV-scale dark matter parameter space.
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Inelastic self-interacting dark matter with small mass splitting produces a cutoff in the matter power spectrum at k > 1 h Mpc^{-1} whose location depends on cross-section normalization, velocity dependence, dark matter mass and mass splitting, yielding non-monotonic exclusion regions from Lyman-α森林
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Solar Reflection of Inelastic Dark Matter
Solar-reflected inelastic dark matter produces detectable signals in xenon and semiconductor detectors, enabling new constraints on MeV-scale dark matter parameter space.
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Cosmology of Inelastic Self-Interacting Dark Matter: Linear Evolution and Observational Constraints
Inelastic self-interacting dark matter with small mass splitting produces a cutoff in the matter power spectrum at k > 1 h Mpc^{-1} whose location depends on cross-section normalization, velocity dependence, dark matter mass and mass splitting, yielding non-monotonic exclusion regions from Lyman-α森林