where C µ is equal to 〈 S 〉 /M 2 ∗ times the order one coefficient. If these states are transferred to the mass eigenstates, further mixing factor must be included. After H 0 d obtains a VEV, we shall have two-body and three-body S decays. Comparing to the two-body S decays, the three-body S decays have an extra factor ( M$_{D}$/ 〈 H 0 d 〉 ) $^{2}$/ (96 π $^{2}$) where m$_{D}$ is the mass of the heavy DM particle S . In our models, we choose M$_{D}$ = 3 TeV and tan β = 30, and then we get ( M$_{D}$/ 〈 H 0 d 〉 ) $^{2}$/ (96 π $^{2}$) ∼ 282, Therefore, we only consider three-body S decays in this paper. The heavy decay DM particle is the scalar component of S , whose three-body on-shell decays are given by the second line of Eq. (17) S → ˜ N$_{3}$$_{,}$$_{4}$µ ˜ µ$_{R}$, ˜ C$_{1}$$_{,}$$_{2}$ν$_{µ}$ ˜ µ$_{L}$, ˜ C$_{1}$$_{,}$$_{2}$µ ˜ ν$_{µ}$$_{L}$, A $^{0}$( H $^{0}$) µµ, C $^{−}$ν$_{µ}$ µ$_{R}$ . (18) With the Eq. (B9) in the Appendix B, we obtain that all these nine primary decay channels almost have the democratic rates except the mixing factor for each channel. Anyway, the total decay rate is given by where I denotes the I -th decay channel in Eq. (18). In our paper, the DM particle S is so heavy that the phase space suppressing factor R$_{I}$ is almost process independent and is a constant around 1/6 (see Eq. (B9)). Then, the scale of the DM S lifetime is estimated to be Γ$_{total}$ = 1 128 π 3 〈 S 〉 $^{2}$m2 D M 4 ∗ ( ∑ I C 2 $_{I}$R$_{I}$ ) × m$_{D}$, (19) τ$_{S}$ ∼ 2 . 7 × 10 26 × ( 3TeV m$_{D}$ ) 3 ( M$_{∗}$ 10 $^{17}$GeV ) 4 ( 3 TeV 〈 S 〉 ) 2 ( 1 ∑ I C 2 $_{I}$R$_{I}$ ) s. (20) The random coefficient of the operator has been set to be 1. Notice that except the last factor, Eq. (20) is the so-called τ$_{eff}$ which is the inverse of Γ$_{eff}$ defined in Eq. (B9). Although the very large astrophysical uncertainties do exist in the calculations of cosmic ray, we do not want to scan all the viable parameter space. We only want to demonstrate that with appropriate parameters, we can explain the PAMELA and FERMI experiments in Model I and explain the PAMELA and ATIC experiments in Model II. A. Cosmic e ± Excess IV. COSMIC RAY ANOMALIES In the Micky Way dark halo, the DM S decays into the SM particles, which propagate to the solar system. The propogation of charged particles is described by diffusion equation. 10