Dark matter for $b\to s \mu^+ \mu^-$ anomaly in a gauged $U(1)_X$ model

We propose a new physics model which has a cold dark matter candidate and can explain the $b \to s \mu^+\mu^-$ anomaly at the same time. Our model includes a scalar quark $\widetilde{q}$ and a scalar lepton $\widetilde{\ell}$ which are $SU(2)_L$-doublet as well as a Dirac fermion $N$ which is $SU(2)_L$-singlet. The new particles are charged under a gauged $U(1)_X$ group which is spontaneously broken to a discrete $Z_2$ symmetry by a dark scalar $S$. The remnant $Z_2$ symmetry stabilizes the dark matter. Box diagrams with $\widetilde{q}$, $\widetilde{\ell}$, and $N$ running inside the loop can generate the correct Wilson coefficients $C_9^\mu = -C_{10}^\mu$ to accommodate the $b \to s \mu^+\mu^-$ anomaly while avoiding constraints such as $B_s-\overline{B}_s$ mixing. The dark matter annihilation into a second generation lepton pair via $t$-channel $\widetilde{\ell}$-exchanging process plays an important role in producing the current dark matter relic abundance of the universe, showing a strong interplay between the flavor and dark matter physics. We also discuss dark-gauge-interaction-dominated and Higgs-portal-dominated scenarios for dark matter physics.


Introduction
Since the LHCb Collaboration reported some deviations from the Standard Model (SM) prediction in the B → K ( * ) ( = e, µ) decays a few years ago [1,2], a lot of interest has been drawn to reveal the origin of the anomalies . The relevant process to the anomalies in the quark level is the b → s transition, which is flavor-changing neutral current (FCNC) and is highly suppressed in the SM. Therefore, the semileptonic B decays would greatly be sensitive to new physics (NP).
The sizable discrepancies reported by the LHCb Collaboration are the ratio, R K ( * ) , of branching ratios of the B decays into K ( * ) , which is defined by with the SM prediction close to unity. R K for the dilepton invariant mass squared range 1 < q 2 < 6 GeV 2 in the B + → K + + − decay has 2.6σ deviation from the SM prediction [1], while the R K * values are deviated from the SM predictions by 2.1-2.3σ and 2.4-2.5σ in the low (0.045 < q 2 < 1.1 GeV 2 ) and high (1.1 < q 2 < 6 GeV 2 ) dilepton invariant mass region, respectively [60]. Another anomaly in the b → s transition reported by the LHCb Collaboration is the differential branching fraction for 1 < q 2 < 6 GeV 2 in the B s → φµ + µ − decay, which is more than 3σ below the SM predictions based on the lightcone sum-rule form factors [61]. Finally, the angular analyses of B → K * + − performed by the LHCb, BELLE, and ATLAS collaborations show about 2 ∼ 3σ deviation for the P 5 observable [2,[62][63][64] while the measurement by the CMS Collaboration is consistent with the SM [65]. These observations may imply hints of NP in the b → s transition. The b → s transition is described by the effective weak Hamiltonian  [66,67]. Global fitting analyses [68][69][70][71][72][73] show that sizable NP contributions to C µ 9 (10) can accommodate the data. We notice that the individual deviations in the observables mentioned above are in the same direction, i.e. destructive with the SM, and when combined, the discrepancy with the SM predictions can be as large as ∼ 5σ [68][69][70][71][72][73].
Best fit values of NP models manifesting in a one-dimensional Wilson coefficient(s) include C µ,NP 9 = −1.21 (5.2σ) and C µ,NP 9 = −C µ,NP 10 = −0.67(4.8σ) [69]. We consider the latter scenario in this paper. The allowed range in this model is (

1.4)
On the other hand, other observables relevant to the b → s transition are well consistent with the SM. For example, the branching fractions of the pure leptonic decay, B s → µ + µ − , and the radiative decay, B → X s γ, agree with the SM estimations. In addition, the forwardbackward asymmetry, A F B , and the quantity, F H , which are defined in the B + → K + µ + µ − decay as dΓ/d cos θ ∼ 3 4 (1 − F H )(1 − cos 2 θ) + 1 2 F H + A F B cos θ, are good agreement with the SM prediction [74]. Especially, the latter disfavors the presence of new (pseudo)scalar operators, O ( ) [75]. In the present article, we propose a NP model with an additional local dark U (1) X symmetry to resolve the anomalies in the b → s transition. We introduce a new vectorlike fermion and several new scalars charged under the U (1) X symmetry as well as the SM gauge symmetry. The SM particles are neutral under the U (1) X symmetry. The new fermion and scalars can interact with the SM fermions through Yukawa interactions and, also, the mixing between the SM Higgs doublet and new scalar singlet. Because the gauge boson of the U (1) X symmetry does not couple to the SM fermions directly, the b → s transition can have effects of NP through box diagrams at the loop level. We find that this model could account for the anomalies in the b → s transition. This model naturally contains a candidate for cold dark matter (DM) due to the remnant Z 2 symmetry after breakdown of the U (1) X symmetry. We find that this model can also explain the relic density of the universe. This paper is organized as follows. In section 2, we construct our model. In section 3 we calculate NP contribution to b → sµµ, B → K ( * ) νν, B s − B s mixing, B s → µ + µ − , b → sγ, the anomalous magnetic moment of muon a µ , and the loop-induced effective Zµ + µ − coupling. In section 4 we consider dark matter phenomenology. Finally we conclude in section 5. Loop functions are collected in appendix A.

The model
In addition to the SM gauge group SU (3) C × SU (2) L × U (1) Y we introduce a local dark U (1) X symmetry under which all the SM fields are neutral. We also introduce new fields which have quantum number assignments as shown in table 1.

New fermion New scalars
The Dirac fermion N has a mass term, It couples to the SU (2) L -doublet scalars q, , and the SM-singlet scalar S, via Yukawa interactions, where i(= 1, 2, 3) is the generation index. We set λ 1 q ≡ 0 to evade strong constraints, e.g., The Yukawa couplings λ 1 and λ 3 are irrelevant to b → sµµ transition, and we set λ 1 ≡ λ 3 ≡ 0 in order not to generate µ → eγ and τ → µ(e)γ processes. The scalar potential is written in the form obtained in (N, N c ) basis, we get the mass eigenstates From (2.9) we can see that the Majorana phases, η ∓ = ∓1, are assigned so that N c ∓ = η ∓ N ∓ . We see that the original Dirac particle N splits into two Majorana fermions N ∓ . It is noted that the VEV v S breaks the original U (1) X symmetry into a remnant discrete Z 2 symmetry under which N ∓ , q, and are odd while all the others are even. By this local discrete symmetry the lightest new particle which we take to be N − with odd parity under the Z 2 symmetry does not decay into any other particles and can play the role of a dark matter candidate.
We can write the SM Higgs H and the dark scalar S in terms of their components in the unitary gauge. The potential V given in the form of (2.4) automatically satisfies the tadpole condition, ∂V /∂h| vacuum = ∂V /∂s| vacuum = 0. The scalar mass-squared matrix is obtained where H 1 is identified with the SM-like Higgs boson with mass m H 1 = 125 GeV. The mixing angle α H is constrained by the LHC Higgs experiments [76,77]. The direct detection experiments of dark matter also constrains this angle through the Higgs portal interaction, λ HS H † HS † S. We take α H ≤ 0.1 in order to avoid these constraints. The quark fields q L = (u L , d L ) T , 1 need to be rotated to be in the mass eigenstates. We assume that the down-type quarks in (2.3) are already in the mass basis and that the flavor mixing due to Cabibbo-Kobayashi-Maskawa (CKM) matrix V appears in the upquark sector, i.e. d L = d L , u L = V † u L with d L , u L being the mass eigenstates. In the mass-eigenstate basis, the Yukawa interactions with quarks are where λ i u = j=1,2,3 V ij λ j q and λ i d = λ i q (i = 1, 2, 3). As a consequence we can see that is induced even if we set λ 1 q ≡ 0. The induced λ 1 u can be constrained, e.g., by D 0 − D 0 mixing. However, due to Cabibbo-suppressed contribution to D 0 − D 0 at least by O(λ 2 C ) with λ C (≈ 0.23) being the Cabibbo angle, the constraint from D 0 − D 0 can be always satisfied once the constraint from B s −B s is imposed [78]. We do not consider this constraint further. The effective Yukawa coupling λ i ν to the i-th neutrino is obtained by a similar procedure with the quark case: λ i e = λ i , λ i ν = U * ji λ j , where U is the Pontecorvo-Maki-Nakagawa-Sakata (PMNS) mixing matrix for neutrino oscillations.
In the new charged-scalar sector, there is mass splitting between u( ν) and d( e) due to λ Since large scalar mass splitting leads large contribution to ρ-parameter [79] and also the mass splitting does not affect our analysis, we set λ ( ) = 0 for simplicity. The kinetic mixing term between Z and Z(γ), − Z µν B µν with B µν being the field strength of the U (1) Y gauge boson, is generally allowed by the gauge symmetry we consider. However, since the mixing does not generate lepton-flavor-violating b → s and the parameter is constrained to be less than 10 −2 for m Z ∼ 100 GeV [80], we set = 0 for simplicity.

NP contribution to b → sµµ transition and constraints on the model
In our model the b → sµ + µ − transition operators O µ 9,10 which can explain the b → sµ + µ − anomaly are generated via the box diagrams shown in figure 1. The arrows represent color or lepton number flow. In the U (1) Lµ−Lτ model considered in [81] the b → sµ + µ − transition operators are generated from penguin diagrams at one-loop level. This clearly distinguishes the current model from the one considered in [81]. The existence of crossed diagrams in the right panel represents the Majorana nature of N ∓ . The resulting C µ,NP 9(10) , however, is not simple algebraic sum of the Majorana contributions presented in the literature, e.g., in [78]. In the limit ∆M ≡ M + − M − → 0, the two Majorana fermions N ∓ merges into a single Dirac fermion N . As a result, the crossed diagrams disappear in this limit due to the restored U (1) X symmetry. This can be clearly seen from the minus sign in front of the second j function in those Wilson coefficients Neglecting the minus sign which originates from the Majorana phase η − = −1, the above results agree with those in [78] up to overall sign. The loop functions k and j are listed in the appendix A. In the limit of degenerate masses we get k(1, 1, 1) = 1/3 and j(1, 1, which is close to the best fit value in (1.4) to solve the b → sµµ anomaly. To emphasise the importance of the wrong sign in (3.1) and also to see the behaviour for large scalar quark/lepton masses, we show a plot of C µ,NP The value |λ 2 q λ 3 * q | is constrained by the B s − B s mixing which will be considered below. As we will show later, a rather large value of λ 2 is required to explain the anomaly. This will also affect the dark matter phenomenology as we will discuss later.
The b → sµµ transition occurs also through γand Z-penguin diagrams. However, since γ and Z couplings to leptons are flavour universal, the penguin contributions should not be too large. We obtain where e d = −1/3 and the loop-function P γ (x) is listed in the appendix A. We note that the above contribution to C 9 is independent of λ 2 and, compared to the box contribution, is suppressed in the case when large λ 2 is required. For the benchmark point, M − = 100 GeV, M + = 200 GeV, and m d = 1 TeV, we get which is 3 orders of magnitude smaller than C µ,NP 9 in (3.2). It is known that the bsZ-vertex is proportional to q 2 with q being the virtual 4-momentum of Z-boson [78]. Since q 2 ∼ m 2 b , the Z-penguin is further suppressed compared with the γ-penguin by a factor q 2 /m 2 Z . Since is SU (2) L doublet, the same box diagrams which generate b → sµµ shown in figure 1 also generate the semi-leptonic decay B → K ( * ) νν. The effective Hamiltonian is We can obtain C 22 L just by replacing m → m ν and λ 2 → λ 2 ν . The effective Yukawa coupling Since neutrino flavors are not measured in the experiments, the total branching ratio normalized to the SM prediction defined by [78] R νν can be compared with the measurements From the inequality, has both the SM contribution and the NP contributions The SM Wilson coefficient at the electroweak scale is where x t = m 2 t /m 2 W and the loop function S 0 (x t ) can be found, e.g., in [82]. The NP contribution from figure 3 reads The Yukawa interactions with couplings λ 2 q and λ 3 q also generate operators O 7γ and O 8g , contributing to a radiative flavor-changing b decay, b → sγ. The experimental measurement and the SM prediction of the inclusive branching fraction of radiative B-decay, B → X s γ, are [83,84] B B → X s γ, (E γ > 1. The NP contribution to C γ 7 at the electroweak scale whose diagram is shown in figure 4 is obtained to be which is at least two orders of magnitude below the current bounds in (3.20). The leptonic decay B s → µ + µ − can be very sensitive to NP models such as Minimal Supersymmetric Standard Model (MSSM) [85][86][87][88][89]. In our model the contributions to the scalar operators, (s L b R )( ), (s L b R )( γ 5 ), are suppressed by small muon mass compared to NP scale. However, since the model explains b → sµµ anomaly in the C 9 = −C 10 scenario, NP contribution to C 10 can be sizeable. The measurement by LHCb collaboration [90] is a little smaller than the SM prediction [91,92] B(B s → µ + µ − ) SM = (3.65 ± 0.23) × 10 −9 , (3.23) although they agree with each other within 1σ. Interestingly the scenario in (1.4) requires positive C µ,NP 10 in the 2σ range whereas C SM 10 is negative, predicting smaller branching fraction than that of the SM as favoured by the LHCb experiment. Using (3.22) and (3.23), we obtain the ratio, The anomalous magnetic moment of muon a µ = (g − 2) µ /2 also receives contribution from the diagram figure 4 with replacement b, s → µ and d → e. The effective Hamiltonian for a µ is We get where y ∓ = M 2 ∓ /m 2 e and the loop function J 1 (y) is listed in appendix A. The difference between the experimental measurement [93] and a most recent SM prediction [94] ∆a µ = a exp µ − a SM µ = (236 ± 87) × 10 −11 , can satisfy the 3σ range in the discrepancy: −25 × 10 −11 ≤ ∆a µ ≤ 497 × 10 −11 . Note that in our model a suppression factor m 2 µ /m 2 e results from the chirality flip in the external muon line.
Additional constraint may come from effective Zµ + µ − vertex which is generated from the diagrams similar to figure 4 but with the replacement: γ → Z, d → e and b, s → µ. The NP contribution g NP L to the effective vertex [95] given by turns out to be finite and proportional to the four-momentum square of Z, q 2 : where y ∓ = M 2 ∓ /m 2 e . The loop function F 9 (y) can be found in the appendix A. The SM contribution at tree level is g SM,tree The LEP experiment measured the coupling g Lµ at Z-pole [96] with the result We impose the constraint which is an order of magnitude below the experimental upper bound (3.33). As we have seen above, the constraint from the B s − B s mixing is the strongest and all the others are orders of magnitude below the current experimental bound. We'll impose only the B s − B s mixing constraint for our numerical analysis. The model is also constrained by collider experiments such as the LHC. The most telltale signature for the model is the observation of new scalar particles. For example, the new colored-scalar particles can be searched for at the LHC via, pp → d d * followed by the decay d → bN − processes, giving b-jets and missing transverse momentum events [97,98]. Using 36.1 fb −1 of pp collision data at √ s = 13 TeV the ATLAS collaboration excludes m d 950 GeV for M − 420 GeV at 95% confidence level [99]. To be conservative we use m q( ) ≥ 1 TeV in the numerical analysis below.

Dark matter phenomenology and numerical results
In this section we discuss dark matter physics such as dark matter relic abundance and direct detection for our dark matter candidate N − . In our model weakly interacting massive particle (WIMP) N − is a good candidate for a thermal dark matter. We assume N − is the only dark matter component. In the early universe the dark matter N − is in thermal equilibrium with the SM plasma through processes, N − N − ↔ SM SM, some of which are shown in figure 5. As the universe cools down and the rates for these processes drop below the expansion rate, the dark matter particle freezes out from the thermal bath. The current relic density can be estimated from Figure 5. Representative diagrams for DM annihilation in scenarios I), II), and III).
We will see that there is strong interplay between b → sµµ anomaly and dark matter phenomenology. The dominant DM interactions include Yukawa interaction with the 2nd generation leptons, dark-gauge interaction, and Higgs portal interaction. We study three benchmark scenarios depending on the dominant interactions contributing to the dark matter annihilation: I) dark-Yukawa-interaction(λ 2 )dominated channels, II) dark-gauge-interaction(g X )-dominated channels and III) Higgsportal(λ HS )-dominated channels. Representative diagrams for each category are shown in figure 5.
In the Scenario I) the diagram of type I) in figure 5 can easily dominate over other channels because we need relatively large λ 2 to explain the b → sµµ anomaly since λ 2 q λ 3 * q is strongly constrained by the mass difference in B s − B s mixing as shown in (3.16). figure 6 shows DM relic density and C µ,NP 9 in (M − , λ 2 )-plane in Scenario I). The red line is a contour line for a constant dark matter relic density Ω DM h 2 = 0.12 [100]. The dark (medium, light) blue region satisfies 1σ(2σ, 3σ) allowed region for C µ,NP We take the rest free parameters as for all scenarios. We note that the direct detection constraint on Scenarios I) is not significant because it first occurs at one-loop process and is also proportional to the momentum transfer to nucleon. To be more specific, let us consider N − q → N − q process mediated by the dominant one-loop N − N − γ vertex inside which µ and e are running. A naive dimensional analysis gives the effective operator where we used the Majorana nature of N − . In the zero momentum transfer limit only the space component of N − γ µ γ 5 N − and the time component of qγ µ q survive. Consequently for non-zero but small momentum transfer, the contribution of the above operator to the direct detection cross section is suppressed by MeV is the maximum momentum transfer to a nucleon [101]. Since this suppression factor Q 2 /M 2 − ∼ 10 −10 (for M − ∼ 100 GeV) is very small, we can safely neglect the contribution to the direct detection. Even if we set λ 1 q ≡ 0, λ 1 u is induced as we saw in (2.14). We may expect the effective uuZ vertex is generated by λ 1 u at one-loop level. It has contribution to the direct detection cross section via the operator which is loop-and CKM-suppressed. Most importantly the DM scattering off the nucleon in this case is inelastic upward scattering which does not occur unless the mass splitting is less than 1 keV: We have also checked that the entire region satisfies bound from the B s − B s mixing which is the strongest flavor constraint. Thus we can explain the b → sµµ anomaly and the correct DM relic abundance of the universe while satisfying the constraints from the flavor physics, astrophysics, and cosmology. In both plots of figure 6 we can see that the N − N − → process in figure 5 I) determines the DM relic abundance in almost all the mass range considered. In the left plot the Ω DM h 2 contour line near M − ≈ M + = 1000 GeV drops abruptly because the coannihilation processes, such as N − N + → Z → * , which do not depend on λ 2 can dominate. In the right plot these coannihilation processes cannot occur due to large mass difference ∆M . The annihilation cross section of N − N − → is p-wave suppressed and is approximately given by [102] where we set m ≡ m ν = m e . For fixed m and λ 2 the above annihilation cross section increases as M − increases, which is the reason the λ 2 is decreasing as M − is increasing along the red lines in figure 6. In scenario II), the Z is lighter than the dark matter and the scalar-quark and scalarlepton are very heavy so that its contribution to the DM annihilation is suppressed. Thus we expect that the type of diagrams in figure 5 II) dominates the DM annihilation. Figure 7 shows plots for DM relic density and C µ,NP and (4.4). We set m Z ≡ M − /2 so that N − N − → Z Z is kinematically allowed. The red-orange line is a contour line for a constant dark matter relic density Ω DM h 2 = 0.12.
GeV) becomes important in the orange segment. Therefore only the line segment with red colour represents Scenario II). The dark (medium) blue region satisfies 1σ(2σ) allowed region for C µ,NP 9 to explain b → sµµ anomaly in (1.4). We note that Ω DM h 2 is almost insensitive to g X as M − increase along the red line segment, as opposed to the naive expectation which dictates the increase of g X to compensate for the increase of M − . This is due to enhancement M 4 − /m 4 Z of the N − N − → Z Z cross section which comes from the longitudinal component of Z [103]. Since C µ,NP 9 mildly depends on M − and does not depend on g X , wide region can explain the b → sµµ anomaly at 1σ level, accommodating the correct DM relic abundance at the same time. As in the case of Scenario I) the direct detection occurs via effective operators of types in (4.5) and (4.6). And the constraint from the direct detection experiments is not significant. Now let us discuss the fate of Z in this scenario. Since Z is not protected by the symmetry, it decays eventually into the SM particles. A main contribution comes from one-loop diagram where N ∓ and are running. A naive estimate for the partial decay width GeV, (4.9) gives the lifetime, ∼ 10 −22 sec, which is much shorter than the age of the universe. If the annihilation cross section of N − N − → Z Z in the current universe is too large, the experiments measuring cosmic rays will impose constraints on the parameter space. To see this more clearly we obtained the expression of σv for t-channel N + -exchanging N − N − → Z Z process: which is much smaller than the Fermi-LAT bound of about 3.0 × 10 −27 cm 3 /s [104]. The annihilation cross section for σv(N − N − → µ − µ + (ν µ ν µ )) in the current universe is very small because it is p-wave suppressed as can be seen from (4.7). The entire region in both plots in figure 7 satisfies the constraint from the B s − B s mixing (3.15). Now let us consider Scenario III) whose typical Feynman diagram for DM annihilation is figure 5 III). A necessary condition that Scenario III) is dominant is to have sizable in (M − , α H )-plane in Scenario III). The red line is a contour line for the constant dark matter relic density Ω DM h 2 = 0.12. The dark (medium) blue region satisfies 1σ(2σ) allowed region for C µ,NP 9 to explain b → sµµ anomaly in (1.4). The gray region is excluded by a recent DM direct detection experiment XENON1T [105]. For the left (right) plot, we take m H2 = 500(300) GeV and g X = 0.5 (2). The other parameters we take can be found in the text.
α H . We also need sizable f , which is not free parameter in our set up but is given by To enhance f we need to enhance g X /m Z , and as a consequence dark gauge interaction (Scenario II)) may interfere with this scenario. Since we also need to explain the b → sµµ anomaly, we need to allow large λ 2 given that λ 2 q λ 3 * q is strongly constrained by B s − B s mixing. This also allows an enhancement of N − N − → process through t-channel -exchange, which may result in the domination of Yukawa interaction λ 2 leading to Scenario I) above. The above analysis tells us that pure Higgs portal scenario may not be possible in our model in case we want to explain the b → sµµ anomaly and dark matter at the same time. The Higgs mixing angle α H is also strongly constrained by the DM direct search experiments such as XENON1T, PANDA, etc.. This can be seen in figure 8. It shows DM relic density and C µ,NP 9 in (M − , α H )-plane in Scenario III). The red line is a contour line for the constant dark matter relic density Ω DM h 2 = 0.12. The dark (medium) blue region satisfies 1σ(2σ) allowed region for C µ,NP 9 to explain b → sµµ anomaly in (1.4). The gray region is excluded by a recent DM direct detection experiment XENON1T [105]. For the left (right) plot, we take m H 2 = 500(300) GeV and g X = 0.5 (2). For this figure we fixed as

350(250)
GeV, the t-channel N − -exchanging process N − N − → H 2 H 2 which is independent of α H becomes important. This explains the abrupt drop of red line near the threshold. As in the case of Scenario II), the b → sµµ anomaly can be easily explained once the correct DM relic density is obtained.

Conclusions
We proposed a new physics model which can explain the recent b → sµµ anomaly and a cold dark matter at the same time. The model has a local dark U (1) X symmetry which is broken spontaneously into a discrete Z 2 symmetry by a dark Higgs scalar S. This local discrete symmetry guarantees the stability of the dark matter. The dark matter candidates N and the new SU (2) L -doublet scalars q and which have the same quantum numbers with the left-handed SU (2) L -doublet quarks and leptons contribute to b → sµµ process via box diagrams.
We considered possible constraints on the model, which include B s − B s mixing, B → K ( * ) νν decay, inclusive B-decay b → sγ, B s → µ + µ − , anomalous magnetic moment of muon a µ , loop-induced effective Zµ + µ − vertex as well as new particle masses from the LHC. We also checked whether the correct dark matter relic abundance can be achieved with the constraint from the dark matter direct detection experiments. We found that the constraint from B s − B s mixing is the strongest in the flavor sector. The b → sµµ anomaly can be explained by assuming a relatively large λ 2 ≈ 2 for TeV new particles while satisfying the B s − B s mixing constraint with λ 2 q λ 3 q ≈ −0.15. Given the large Yukawa coupling λ 2 ≈ 2, the t-channel N − N − → plays an important role in achieving the current relic abundance of the universe, showing a strong interplay between apparently unrelated flavor and dark matter physics. When Z is lighter than the dark matter and the dark gauge coupling g X is sizable, N − N − → Z Z can also become dominant. These two dark matter annihilation processes are not strongly constrained by the dark matter direct detection experiments because the dark matter scattering with the nucleon processes occur first at one-loop level and are suppressed by the dark matter Yukawa coupling with the first generation quarks. On the other hand the Higgs portal interaction can play important role to generate the current dark matter relic only near the resonance region and is strongly constrained by the direct detection experiments, restricting the mixing angle of the SM Higgs and dark Higgs α H 0.01.