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<img src='content_image/328251.jpg'>

decay. Moreover, it predicts a continuously going up trend until arriving at the peak around 0.5 TeV, which can be tested by the upcoming PAMELA experiment. 

## B. Anti-Proton Fluxes 

Bcause Higgs bosons and charginos can couple to the SM quarks, their decays may produce anti-proton excess as well. However, the anti-proton excess is not observed by the PAMELA experiment. The propagation of anti-proton is similar to that of positron, but it is simpler by the virtue of no energy loss process from the inverse Compton scattering 

<img src='content_image/328249.jpg'>

However, the Milky Way’s galactic wind ⃗ V$_{c}$ ( ⃗ x ), which is usually assumed along the z axial direction and then is reduced to V$_{c}$ sign( z ) ⃗ k , induces the drift of anti-protons during prop- agation, as reflected in the third term. The last term represents the annihilations between the anti-protons and interstellar protons in the galactic plane, whose thickness is about h ≈ 0 . 1 kpc ≪ L , the half-thickness of cylinder diffusion region of charged particles. The 

