  Excesses on positron and electron fluxes measured by ATIC, and the PAMELA and
Fermi--LAT telescopes can be explained by dark matter annihilation in our
Galaxy. However, this requires large boosts on the dark matter annihilation
rate. There are many possible enhancement mechanisms, such as the Sommerfeld
effect or the existence of dark matter clumps in our halo. If enhancements on
the dark matter annihilation cross section are taking place, the dark matter
annihilation in the core of the Earth should also be enhanced. Here we use
recent results from the IceCube 40-string configuration to probe generic
enhancement scenarios. We present results as a function of the dark
matter-proton interaction cross section, $\sigma_{\chi p}$ weighted by the
branching fraction into neutrinos, $f_{\nu\bar{\nu}}$, as a function of a
generic boost factor, $B_F$, which parametrizes the expected enhancement of the
annihilation rate. We find that dark matter models which require annihilation
enhancements of $\mathcal{O}(100)$ or more and that annihilate significantly
into neutrinos are excluded as the explanation for these excesses. We also
determine the boost range that can be probed by the full IceCube telescope.
