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Cosmic rays interacting in the solar atmosphere produce showers that resultin a flux of high-energy neutrinos from the Sun. These form an irreduciblebackground to indirect solar WIMP co-annihilation searches, which look forheavy dark matter particles annihilating into final states containing neutrinosin the Solar core. This background will eventually create a sensitivity floorfor indirect WIMP co-annihilation searches analogous to that imposed bylow-energy solar neutrino interactions for direct dark matter detectionexperiments. We present a new calculation of the flux of solar atmosphericneutrinos with a detailed treatment of systematic uncertainties inherent insolar atmospheric shower evolution, and we use this to derive the sensitivityfloor for indirect solar WIMP annihilation analyses. We find that the floorlies less than one order of magnitude beyond the present experimental limits onspin-dependent WIMP-proton cross sections for some mass points, and that thehigh-energy solar atmospheric neutrino flux may be observable with running andfuture neutrino telescopes.

Solar Atmospheric Neutrinos and the Sensitivity Floor for Solar Dark Matter Annihilation Searches