WIMP annihilation as well as the production modes of the final state charged particles. If the mediators have a typical decay length on the order of the solar radius or slightly less, processes such as absorption and reflection have the potential to strongly degrade the overall signal flux, and the strong solar magnetic fields may drastically alter the trajectories of the charged particles. If the mediator escapes and decays well past the solar radius, the effects of the heliosphere and the Earth’s magnetosphere can be still be significant, especially for less energetic particles in the tens of GeV range and below (where the bulk of the anomalous PAMELA positrons reside).

We must emphasize that the main feature of this signal would be a high degree of anisotropy in the predicted flux of electrons and positrons, correlated with the center of the sun, which should make this scenario testable. An important consideration is to what degree this tight correlation may be affected or degraded through the processes discussed above. It is instructive to compare this signal with a possible pulsar component to the rising positron fraction of PAMELA [@pulsar], where one of the main signatures may again be an anisotropic signal. 