I. INTRODUCTION It is well known that supersymmetry privides an elegant solution to gauge hierarchy problem in the Standard Model (SM). In the Minimal Supersymmetric Standard Model (MSSM), gauge coupling unification can be realized, which give us the important hint of Grand Unified Theory (GUT). In addition, in the supersymmetric SMs, we can define a Z$_{2}$ symmetry called R parity under which the SM particles are even while their supersymmetric partners are odd. With R parity, we can avoid the dimension-four proton decay problem and evade the stringent constraints from the electroweak precision data naturally. Interestingly, the lightest supersymmetric particle (LSP) is stable due to the R parity, and then can be the dark matter (DM) candidate. For example, the lightest neutralino can be a viable cold DM candidate, which can give us the correct relic density as well. During the last two years, there were quite a few very interesting DM experiments from indirect and direct dections. The ATIC [1] and PPB-BETS [2] collaborations have reported the measurements of cosmic ray (CR) electron/positron spectra at energies up to ∼ 1 TeV. These data show an obvious excess over the expected background in the energy ranges ∼ 300 − 800 GeV and ∼ 500 − 800 GeV, respectively. In the mean time, the PAMELA collaboration also released their first CR measurements of the positron fraction [3] and the ¯ p/p ratio [4]. Although the ¯ p/p ratio is consistent with the astrophysical expectation from the interactions between the CR nuclei and interstellar medium, the positron fraction indeed shows a significant excess for energies above 10 GeV up to ∼ 100 GeV, compared to the background predicted by the conventional CR propagation models. Later, the Fermi-LAT collaboration has released data on the measurement of the electron/positron spectrum from 20 GeV to 1 TeV with unprecedented precision [5], and the HESS collaboration has released the data on the measurements of electron/positron spectrum from 340 GeV to 700 GeV [6], complementing their earlier measurements from 700 GeV to 5 TeV [7]. For simplicity, we will denote the Fermi-LAT collaboration as FERMI collaboration in the following. Although the corresponding data from the ATIC and the FERMI/HESS experiments are not fully consistent, it was shown that the DM models, where the DM particles annihilate or decay dominantly to the SM leptons, can explain these experiments by choosing the suitable DM particle mass and the proper final state particles. To explain the PAMELA/ATIC experiments or the PAMELA/FERMI/HESS experi- ments from DM annihilations, we know that a large boost factor about 100-1000 is needed. However, from astrophysics, the N-body simulation shows that the boost factor from DM substructure can never be larger than 10 [8]. To solve this problem, one can consider the Sommerfield enhancement [9–11] or Breit-Wigner resonant enhancement [12]. Alternatively, we can also consider the non-thermal dark matter production so that the DM annihilation 2