CHAMP Cosmic Rays

We study interactions of cosmological relics, X, of mass m and electric charge qe in the galaxy, including thermalization with the interstellar medium, diffusion through inhomogeneous magnetic fields and Fermi acceleration by supernova shock waves. We find that for m 1010 q GeV, there is a large flux of accelerated X in the disk today, with a momentum distribution 1/p2.5 extending to (β p)max ~ 5 ×104 q GeV. Even though acceleration in supernova shocks is efficient, ejecting X from the galaxy, X are continually replenished by diffusion into the disk from the halo or confinement region. For m 1010 q GeV, X cannot be accelerated above the escape velocity within the lifetime of the shock. The accelerated X form a component of cosmic rays that can easily reach underground detectors, as well as deposit energies above thresholds, enhancing signals in various experiments. We find that nuclear/electron recoil experiments place very stringent bounds on X at low q; for example, X as dark matter is excluded for q > 10−9 and m < 105 GeV. For larger q or m, stringent bounds on the fraction of dark matter that can be X are set by Cherenkov and ionization detectors. Nevertheless, very small q is highly motivated by the kinetic mixing portal, and we identify regions of (m,q) that can be probed by future experiments.

Note:

56 pages, 20 figures. Matches published version. Added discussion on EDGES result, clarifications, and references

supernova: shock waves
charge: electric
electron: recoil
mixing: kinetic
charged particle: massive
cosmic radiation
acceleration
dark matter
diffusion
galaxy

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