FIG. 2: The FERMI data fitting in Model I and the ATIC data fitting in Model II. 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. 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 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 14 ∂ψ ∂t − ∇ · ( K ( ⃗ x, E ) ∇ ψ ) + ∇ · ( ⃗ V$_{c}$ ( ⃗ x ) ψ ) = q ( ⃗ x, E ) − 2 hδ ( z )Γ$_{ann}$ ψ . (28) B. Anti-Proton Fluxes 0.008 0.01 0.02 0.03 10 100 1000 FERMI+PAMELA fit ATIC+PAMELA fi t FERMI-LAT ATIC08 HESS09 background