Stringy WIMP Detection and Annihilation
We calculate the direct dark matter detection spin-independent and proton spin-dependent cross-sections for a semi-realistic intersecting 6-brane model. The cross-sections are compared to the latest constraints of the current dark matter direct detection experiments, as well as the projected results of future dark matter experiments. The allowed parameter space of the intersecting 6-brane model is shown with all current experimental constraints, including those regions satisfying the WMAP and Supercritical String Cosmology (SSC) limits on the dark matter density in the universe. Additionally, we compute the indirect detection gamma-ray flux resulting from neutralino annihilation for the 6-brane model and compare the flux to the projected sensitivity of the Fermi Gamma-ray Space Telescope. Finally, we compute the direct and indirect detection cross-sections as well as the gamma-ray flux resulting from WIMP annihilations for the one-parameter model for comparison, where the one-parameter model is a highly constrained subset of the mSUGRA parameter space such that the soft supersymmetry breaking terms are functions of the common gaugino mass, which is common to many string compactifications.
Observations in cosmology and astrophysics suggest the presence of a stable dark matter particle. Supersymmetry (SUSY) supplies a satisfactory candidate for a dark matter particle, where R-parity is conserved and the lightest supersymmetric particle (LSP) is stable Ellis:1983ew (), which is usually the lightest neutralino Ellis:1983ew (); Goldberg:1983nd (). Two proposed methods of discovering this weakly interacting massive particle (WIMP) are directly through WIMP interactions with ordinary matter and indirectly via the products of WIMP annihilations. The direct detection method searches for elastic scattering of WIMPs off nuclei in underground experiments. The experiments are conducted in deep underground laboratories in an effort to reduce the background to minimal levels. The indirect detection method seeks out debris resulting from WIMP annihilations in the galactic halo. One galactic process that could produce gamma-rays from WIMP annihilation is the process , where two gamma-rays are produced directly from a WIMP annihilation, and another is . Analyses of direct detection cross-sections and gamma-ray flux within mSUGRA (or CMSSM) models have been completed Baltz:2004aw (); Ellis:2005mb (); Roszkowski:2007fd (); Baer:2004qq (). It is, however, a worthwhile pursuit to analyze the direct and indirect detection parameters in alternative models.
The last few years have seen a great deal of interest in Type II string compactifications. Indeed, intersecting D-brane models (see Blumenhagen:2005mu () and Blumenhagen:2006ci () for reviews) on Type II orientifolds have become particularly attractive. In contrast to the standard framework, mSUGRA, the supersymmetry-breaking soft terms for intersecting D-brane models are in general non-universal Kors:2003wf (). Despite substantial progress in constructing such models, most supersymmetric D-brane models suffer from two significant problems. One problem is the lack of gauge coupling unification at the string scale, and the other is the rank one problem in the Standard Model (SM) fermion Yukawa matrices which prevents the generation of mass for the first two generations of quarks and leptons. Nevertheless, there is known one example of an intersecting 6-brane model constructed in Type IIA theory on the orientifold where these problems have been resolved Cvetic:2004ui () Chen:2006gd (). This model exhibits automatic gauge coupling unification at the tree-level and it is also possible to obtain the correct Yukawa mass matrices for both up and down-type quarks and leptons for specific values of the moduli VEVs Chen:2007px () Chen:2007zu (). Furthermore, the soft-supersymmetry breaking terms for this model have been calculated, where regions in the parameter space were discovered that generate the observed dark matter density and satisfy current experimental constraints Chen:2007px () Chen:2007zu (). Although this model has many appealing phenomenological features, one issue still to be completely resolved is that of moduli stabilization. This issue has been addressed to an extent Chen:2006gd () Chen:2007af () by turning on fluxes, but there is still the task of stabilizing the open-string moduli associated with D-brane positions in the internal space and Wilson lines. Only once the moduli stabilization issue has been completely addressed can this model be considered fully realistic.
In this work we show the parameter space allowed by all the experimental constraints for this intersecting 6-brane model for varying cases of gravitino masses and tan. The spin-independent cross-sections are computed and plotted against the current dark matter detection experiment constraints. Furthermore, we present the proton spin-dependent cross-sections, whereas the computed neutron spin-dependent cross-sections only vary slightly from those of the proton, so the neutron cross-sections are not shown. The gamma-ray flux resulting from neutralino annihilations in the galactic halo for the 6-brane model is plotted and compared to the most recent telescope measurements. Finally, in order to compare our results with a model with universal soft terms representing the opposite extreme, we calculate the spin-independent and spin-dependent cross-sections for the so-called one-parameter model Lopez:1993rm (); Lopez:1994fz (); Lopez:1995hg (); Maxin:2008kp (), including the gamma-ray flux. The one-parameter model is a highly constrained small subset of the mSUGRA parameter space such that the soft supersymmetry breaking terms are all functions of the common gaugino mass. In no-scale supergravity models, generically and , thus the number of free parameters is reduced to two, and tan. Adopting a strict no-scale framework, one can also fix the -parameter as , and hence we are led to a one-parameter model where all of the soft terms may be fixed in terms of . Therefore, the one-parameter model represents a suitable case with which to compare the intersecting 6-brane model with non-universal soft supersymmetry breaking terms.
Ii Low-Energy Effective Action
In this section, we give a background discussion for the more technically-minded reader which describes the way in which the supersymmetry breaking soft terms are calculated for intersecting -brane models. In recent years, intersecting D-brane models have provided an exciting approach toward constructing semi-realistic vacua. To summarize, D6-branes (in Type IIA) fill three-dimensional Minkowski space and wrap 3-cycles in the compactified manifold, with a stack of branes having a gauge group (or in the case of ) in its world volume. The 3-cycles wrapped by the D-branes will in general intersect multiple times in the internal space, resulting in a chiral fermion in the bifundamental representation localized at the intersection between different stacks. The multiplicity of such fermions is then given by the number of times the 3-cycles intersect. Due to orientifolding, for every stack of D6-branes we must also introduce its orientifold images. Thus, the D6-branes may also have intersections with the images of other stacks, also resulting in fermions in bifundamental representations. Each stack may also intersect its own images, resulting in chiral fermions in the symmetric and antisymmetric representations. In addition, there are constraints that must be satisfied for the consistency of the model, namely the requirement for Ramond-Ramond tadpole cancellation and to have a spectrum with supersymmetry.
To discuss the low-energy phenomenology we start from the low-energy effective action. From the effective scalar potential it is possible to study the stability Blumenhagen:2001te (), the tree-level gauge couplings CLS1 (); Shiu:1998pa (); Cremades:2002te (), gauge threshold corrections Lust:2003ky (), and gauge coupling unification Antoniadis:Blumen (). The effective Yukawa couplings Cremades:2003qj (); Cvetic:2003ch (), matter field Kähler metric and soft-SUSY breaking terms have also been investigated Kors:2003wf (). A more detailed discussion of the Kähler metric and string scattering of gauge, matter, and moduli fields has been performed in Lust:2004cx (). Although turning on Type IIB 3-form fluxes can break supersymmetry from the closed string sector Cascales:2003zp (); MS (); CL (); Cvetic:2005bn (); Kumar:2005hf (); Chen:2005cf (), there are additional terms in the superpotential generated by the fluxes and there is currently no satisfactory model which incorporates this. Thus, we do not consider this option in the present work. In principle, it should be possible to specify the exact mechanism by which supersymmetry is broken, and thus to make very specific predictions. However, for the present work, we will adopt a parametrization of the SUSY breaking so that we can study it generically.
The supergravity action depends upon three functions, the holomorphic gauge kinetic function, , K\a”ahler potential , and the superpotential . Each of these will in turn depend upon the moduli fields which describe the background upon which the model is constructed. The holomorphic gauge kinetic function for a D6-brane wrapping a calibrated three-cycle is given by (see Blumenhagen:2006ci () for a detailed discussion and explanation of the notation)
In terms of the three-cycle wrapped by the stack of branes, we have
where and are the wrapping numbers of the D-branes on the th two-torus, from which it follows that
where for and for or gauge groups and where we use the and moduli in the supergravity basis. In the string theory basis, we have the dilaton , three Kähler moduli , and three complex structure moduli Lust:2004cx (). These are related to the corresponding moduli in the supergravity basis by
and is the four-dimensional dilaton. To second order in the string matter fields, the K\a”ahler potential is given by
The untwisted moduli , are light, non-chiral scalars from the field theory point of view, associated with the D-brane positions and Wilson lines. These fields are not observed in the MSSM, and if present in the low energy spectra they may disrupt the gauge coupling unification. Clearly, these fields must get a large mass through some mechanism. One way to accomplish this is to require the D-branes to wrap rigid cycles, which freezes the open string moduli Blumenhagen:2005tn ().
For twisted moduli arising from strings stretching between stacks and , we have , where is the angle between the cycles wrapped by the stacks of branes and on the torus respectively. Then, for the K\a”ahler metric in Type IIA theory we find the following two cases:
For branes which are parallel on at least one torus, giving rise to non-chiral matter in bifundamental representations (for example, the Higgs doublets), the K\a”ahler metric is
The superpotential is given by
while the minimum of the F part of the tree-level supergravity scalar potential is given by
where and , is inverse of , and the auxiliary fields are given by
Supersymmetry is broken when some of the F-terms of the hidden sector fields acquire VEVs. This then results in soft terms being generated in the observable sector. For simplicity, it is assumed in this analysis that the -term does not contribute (see Kawamura:1996ex ()) to the SUSY breaking. Then the goldstino is absorbed by the gravitino via the superHiggs effect. The gravitino then obtains a mass
which we will take to be 500 GeV and 700 GeV in the following. The normalized gaugino mass parameters, scalar mass-squared parameters, and trilinear parameters respectively may be given in terms of the K\a”ahler potential, the gauge kinetic function, and the superpotential as
where is the K\a”ahler metric appropriate for branes which are parallel on at least one torus, i.e. involving non-chiral matter.
The above formulas for the soft terms depend on the Yukawa couplings, via the superpotential. An important consideration is whether or not this should cause any modification to the low-energy spectrum. However, this turns out not to be the case since the Yukawas in the soft term formulas are not the same as the physical Yukawas, which arise from world-sheet instantons and are proportional to , where is the world-sheet area of the triangles formed by a triplet of intersections at which the Standard Model fields are localized. The physical Yukawa couplings in Type IIA depend on the K\a”ahler moduli and the open-string moduli. This ensures that the Yukawa couplings present in the soft terms do not depend on either the complex-structure moduli or dilaton (in the supergravity basis). Thus, the Yukawa couplings will not affect the low-energy spectrum in the case of -moduli dominant and mixed and dominant supersymmetry breaking.
To determine the SUSY soft breaking parameters, and therefore the spectra of the models, we introduce the VEVs of the auxiliary fields Eq. (11) for the dilaton, complex and Kähler moduli Brignole:1993dj ():
The factors and are the CP violating phases of the moduli, while the constant is given by
The goldstino is absorbed into the gravitino by in field space, and parameterize the goldstino direction in space, where . The goldstino angle determines the degree to which SUSY breaking is being dominated by the dilaton and/or complex structure () and Kähler () moduli. As suggested earlier, we will not consider the case of -moduli dominant supersymmetry breaking, since in this case the soft terms are not independent of the Yukawa couplings.
Iii Parameter Space and Supersymmetry Spectra
The set of soft terms at the unification scale are generated in the same manner as was performed in Chen:2007zu () for u-moduli dominated SUSY breaking. The soft terms are then input into MicrOMEGAs 2.0.7 Belanger:2006is () using SuSpect 2.34 Djouadi:2002ze () as a front end to run the soft terms down to the electroweak scale via the Renormalization Group Equations (RGEs) and then to calculate the corresponding relic neutralino density. We take the top quark mass to be GeV :2008vn (), and leave tan as a free parameter while is determined by the requirement of radiative electroweak symmetry breaking (REWSB). However, we do take as suggested by the results of for the muon. The results are then filtered according to the following criteria:
The WMAP 5-year data Hinshaw:2008kr () for the cold dark matter density, 0.1109 0.1177. We also consider the WMAP 2 results Spergel:2006hy (), 0.095 0.129. In addition, we look at the SSC model Antoniadis:1988aa () for the dark matter density, in which a dilution factor of (10) is allowed Lahanas:2006hf (), where 1.1. For a discussion of the SSC model within the context of mSUGRA, see Dutta:2008ge (). We investigate two cases, one where a neutralino LSP is the dominant component of the dark matter and another where it makes up a subdominant component such that 0 0.1177, 0 0.129, and 0 1.1. This allows for the possibility that dark matter could be composed of matter such as axions, cryptons, or other particles.
The experimental limits on the Flavor Changing Neutral Current (FCNC) process, . The results from the Heavy Flavor Averaging Group (HFAG) Barberio:2007cr (), in addition to the BABAR, Belle, and CLEO results, are: . There is also a more recent estimate Misiak:2006zs () of . For our analysis, we use the limits , where experimental and theoretical errors are added in quadrature.
The anomalous magnetic moment of the muon, . For this analysis we use the 2 level boundaries, Bennett:2004pv ().
The process where the decay has a dependence. We take the upper bound to be :2007kv ().
The LEP limit on the lightest CP-even Higgs boson mass, GeV Barate:2003sz ().
A scan of the parameter space allowed by the aforementioned five experimental constraints was performed for various values of the gravitino mass and tan, with the goal to determine the range of the gravitino mass where the upper limit is the mass at which SUSY events become observable at the Large Hadron Collider (LHC) above the SM background, and at the lower limit the Higgs mass becomes too light and violates the LEP constraint. We discover the upper limit to be 700 GeV and the lower limit to be in the range = 400 500 GeV. Thus, we calculate the relic density, experimental constraints, and subsequently, the direct detection cross-sections and indirect detection gamma-ray flux for = 500 GeV and = 700 GeV. For each of these gravitino masses, the calculations were completed for tan = 10, 25, and 46. Regions of the parameter space satisfying all the experimental constraints exist for five of the six cases; only = 700 GeV, tan = 10 produced no regions that satisfied the constraints. Additional values of tan were run for = 700 GeV, though tan = 25 is close to the minimum tan that violates none of the constraints. Thus, we study five cases in this paper: = 500 GeV and tan = 10, = 500 GeV and tan = 25, = 500 GeV and tan = 46, = 700 GeV and tan = 25, = 700 GeV and tan = 46.
We plot the parameter space in terms of the goldstino angles and in Fig. 1. A detailed discussion of the goldstino angles and and how they relate to the non-universal gaugino masses and scalar masses can be found in Chen:2007px () Chen:2007zu (). The different shades represent the regions which are allowed or excluded for the reasons noted in the chart legend. These plots focus on the experimental constraints and the dark matter density within the SSC and WMAP regions. Note the small regions excluded by the Higgs mass 114 GeV satisfy all other constraints, including the SSC dark matter density. All the regions in the allowed parameter space pass the Higgs mass constraint, except as just noted, however, it is not identified on the charts whether the excluded regions meet or fail the higgs mass constraint, though all the excluded regions fail to meet one or more of the remaining constraints. In addition, the regions excluded by 1.1 satisfy all other constraints. The circular region centered at the origin of the plot is excluded for driving to negative values. The region outside the allowed parameter space is excluded since the goldstino angles , , and do not satisfy the unitary condition Chen:2007px () Chen:2007zu (). For more explicit details of the parameter space regions satisfying the experimental constraints, including potential LHC signatures and experimental observables, see JMMN (). In the remainder of this work, we focus only on the direct and indirect detection parameters.
Iv WIMP Detection
Direct detection experiments search for dark matter through an elastic collision of WIMPs with ordinary matter. The lightest neutralino, , is assumed to be stable, and as such represents the best possible candidate for dark matter, and hence, WIMPs. These WIMPs produce low energy recoils with nuclei. The interaction between the WIMPs and nuclei can be segregated into a spin-independent (SI) part and a spin-dependent(SD) part, where the SI (scalar) interactions are primarily the consequence of elastic collisions with heavy nuclei. First, we consider the SI cross-sections for an intersecting 6-brane model, then study the SD interactions.
Both the direct detection cross-sections and the gamma-ray flux are calculated using MicrOMEGAs 2.1 Belanger:2008sj (). For the SI calculation, we use the nucleon form factor coefficient values of
while for the SD computations, we use the following quark density coefficients
In addition, we use km/s for the dark matter velocity distribution in the galaxy rest frame, km/s for the Earth velocity with respect to the galaxy, and km/s for the maximal dark matter velocity in the sun’s orbit with respect to the galaxy.
In Fig. 2, we plot the SI cross-sections for an intersecting 6-brane model. The cross-sections and flux were calculated only for those regions of the parameter space satisfying all the experimental constraints. Those allowed regions are shown in Fig. 1. The plots in Fig. 2 are subdivided by dark matter density, where for clarity we use the 2 WMAP limits. The most recent experimental results for Zeplin-III Lebedenko:2008gb (), Xenon 10 Angle:2007uj (), and CDMS II Ahmed:2008eu () are shown, in addition to the projected sensitivity of the future SuperCDMS Schnee:2005pj () and Xenon-1 Ton Aprile:2005mz () experiments. Only for = 500 GeV and tan = 10 are the cross-sections within the current experimental limits, however, in this case there is only a small region of the allowed parameter space within the latest CDMS results, where these points have a very small dark matter density only allowed since we removed the lower WMAP 2 boundary. Most of the points will be within the experimental limits of the SuperCDMS and Xenon-1 Ton future experiments, potentially providing incentive for the design and development of the next generation of dark matter direct detection experiments. In the SSC region, we allow for a dilution factor of (10), resulting in a dark matter density up to , permitting the inclusion of more points. As can be seen in Fig. 2, in general, the SSC regions have a smaller cross-section than the WMAP regions. The dark matter density is inversely proportional to the annihilation cross-section , so one expects the points with a higher to possess a smaller annihilation cross-section, as depicted in Fig. 2.
The proton SD cross-sections are shown in Fig. 3. The format of the SD charts is similar to the SI charts. For comparison of the intersecting 6-brane model cross-sections to the current experimental limits, we show the latest results for COUPP COUP (), NAIAD NAIA (), KIMS Lee.:2007qn (), and SuperK Desai:2004pq (). We also calculated the neutron SD cross-sections (not shown), though there was only a slight difference between the proton and neutron SD. The patterns were generally the same, but the neutron SD cross-sections were slightly larger, and the shape of the SD patterns is essentially identical to the SI patterns. None of the intersecting 6-brane model points are within the current experimental limits of the SD dark matter detectors, and in fact, they are still three orders of magnitude away from the discovery region. Again, since , we see in Fig. 3 that the SSC points have in general a smaller annihilation cross-section than the WMAP points.
V Indirect Dark Matter Detection
Indirect detection experiments search for high energy neutrinos, gamma-rays, positrons, and anti-protons emanating from neutralino annihilation in the galactic halo and core, or in the case of neutrinos, in the core of the sun or the earth. In this work, we focus only on the flux of gamma-rays in the galactic core or halo. The gamma-ray flux for the intersecting 6-brane model is shown in Fig. 4, including the projected sensitivity of the Fermi experiment Morselli:2002nw (). The sensitivity is not constant, but is a function of photon energy, and for this reason, to be precise, we delineate it using a band. Most of the points allowed by the experimental constraints will be within the sensitivity of the Fermi telescope. As mentioned in the Introduction, two possible decay channels where WIMPs can produce gamma-rays in the galactic core and halo are and . Hence, the flux of gamma-rays is directly dependent upon the annihilation cross-section. Fig. 2 and Fig. 3 show and we have explained that the SSC points have a smaller annihilation cross-section. Consequently, we expect the SSC points to also exhibit a smaller gamma-ray flux , and accordingly, this is illustrated in Fig. 4.
It is an intriguing question as to how a model with non-universal soft-supersymmetry breaking terms, such as an intersecting 6-brane model, compares to a model with universal soft-supersymmetry breaking terms, for example, mSUGRA. The one-parameter model (OPM) Lopez:1993rm (); Lopez:1994fz (); Lopez:1995hg (); Maxin:2008kp () is a highly constrained small subset of mSUGRA, where all the soft-supersymmetry breaking terms may be fixed in terms of the gaugino mass . The OPM has universal soft-supersymmetry breaking terms, so it is ideal to compare to the 6-brane model. Details of the phenomenology of the OPM using the most recent measurements of the experimental constraints can be found in Maxin:2008kp (). The parameter space of the OPM is quite constrained by the experimental constraints, and this leads to small regions of allowed direct and indirect detection parameters. In Fig. 5 we plot the direct and indirect detection parameters of the OPM. As described in Maxin:2008kp (), the range of tan for spectra that satisfy all the experimental constraints in the WMAP region is 35.2 tan 38, while the range in the SSC region is 10.2 tan 38. Note that the points shown in Fig. 5 are for all tan within the aforementioned ranges. However, it can be concluded from Fig. 5 that the points with the same WIMP mass do exhibit the same characteristics as the points in the intersecting 6-brane model. For the same WIMP mass, the WMAP spectra have a larger annihilation cross-section, and hence, gamma-ray flux than the SSC points, due to the fact that in the WMAP region, we are not allowing for the (10) dilution factor to .
Much advancement has been made in the last few years toward the discovery of dark matter. Current generation direct detection experiments that search for elastic collisions of WIMPs off nuclei have come within shouting distance of the allowed parameter space of models with universal soft-supersymmetry breaking terms such as mSUGRA. Furthermore, the Fermi Gamma-ray space telescope is edging closer to the parameter space of these same models. In light of this experimental progress, it is a good time to start examining the direct and indirect detection parameters of semi-realistic string models. To this end, we began an investigation of the experimental detection parameters for a particular string-derived model with many appealing phenomenological properties. There are various theoretical models currently offered, so our goal is present the phenomenology of a promising new model, in contrast to the usual standard, mSUGRA. In this work, we investigated an intersecting 6-brane model on a Type IIA orientifold that overcomes the persistent problems experienced by many Type II string vacua, namely that of gauge coupling unification and the generation of masses for the first two generations of quarks and leptons. This model exhibits automatic gauge coupling unification and allows the correct masses and mixings for all quarks and leptons to be obtained. As a consequence, we presented the spin-independent and proton spin-dependent cross-sections. We find that only a small region of the allowed parameter space is within the current limits of the direct detection experiments. Regions with a larger have smaller cross-sections, thus cross-sections for SSC are smaller than those of WMAP. Additionally, we illustrated the galactic gamma-ray flux for this model resulting from neutralino annihilations. We discover that most of the regions of the 6-brane model allowed parameter space will be within the sensitivity of the Fermi telescope.
This research was supported in part by the Mitchell-Heep Chair in High Energy Physics (CMC), by the Cambridge-Mitchell Collaboration in Theoretical Cosmology, and by the DOE grant DE-FG03-95-Er-40917.
- (2) J. R. Ellis, J. S. Hagelin, D. V. Nanopoulos and M. Srednicki, Phys. Lett. B 127, 233 (1983); J. R. Ellis, J. S. Hagelin, D. V. Nanopoulos, K. A. Olive and M. Srednicki, Nucl. Phys. B 238, 453 (1984);
- (3) H. Goldberg, Phys. Rev. Lett. 50, 1419 (1983).
- (4) E. A. Baltz and P. Gondolo, JHEP 0410, 052 (2004) [arXiv:hep-ph/0407039].
- (5) J. R. Ellis, K. A. Olive, Y. Santoso and V. C. Spanos, Phys. Rev. D 71, 095007 (2005) [arXiv:hep-ph/0502001].
- (6) L. Roszkowski, R. Ruiz de Austri and R. Trotta, JHEP 0707, 075 (2007) [arXiv:0705.2012 [hep-ph]].
- (7) H. Baer, A. Belyaev, T. Krupovnickas and J. O’Farrill, JCAP 0408, 005 (2004) [arXiv:hep-ph/0405210].
- (8) R. Blumenhagen, M. Cvetic, P. Langacker and G. Shiu, Ann. Rev. Nucl. Part. Sci. 55, 71 (2005) [arXiv:hep-th/0502005].
- (9) R. Blumenhagen, B. Kors, D. Lust and S. Stieberger, Phys. Rept. 445, 1 (2007) [arXiv:hep-th/0610327].
- (10) B. Kors and P. Nath, Nucl. Phys. B 681, 77 (2004) [arXiv:hep-th/0309167].
- (11) M. Cvetic, T. Li and T. Liu, Nucl. Phys. B 698, 163 (2004) [arXiv:hep-th/0403061].
- (12) C. M. Chen, T. Li and D. V. Nanopoulos, Nucl. Phys. B 740, 79 (2006) [arXiv:hep-th/0601064].
- (13) C. M. Chen, T. Li, V. E. Mayes and D. V. Nanopoulos, Phys. Lett. B 665, 267 (2008) [arXiv:hep-th/0703280].
- (14) C. M. Chen, T. Li, V. E. Mayes and D. V. Nanopoulos, Phys. Rev. D 77, 125023 (2008) [arXiv:0711.0396 [hep-ph]].
- (15) C. M. Chen, T. Li, Y. Liu and D. V. Nanopoulos, Phys. Lett. B 668, 63 (2008) [arXiv:0711.2679 [hep-th]].
- (16) J. L. Lopez, D. V. Nanopoulos and A. Zichichi, Phys. Lett. B 319, 451 (1993) [arXiv:hep-ph/9306226].
- (17) J. L. Lopez, D. V. Nanopoulos and A. Zichichi, Int. J. Mod. Phys. A 10, 4241 (1995) [arXiv:hep-ph/9408345].
- (18) J. L. Lopez, D. V. Nanopoulos and A. Zichichi, Phys. Rev. D 52, 4178 (1995) [arXiv:hep-ph/9502414]. For a review, see Searching for the Superworld: A Volume in Honor of Antonino Zichichi on the Occasion of the Sixth Centenary Celebrations of the University of Turin, Italy, Antonino Zichichi, Sergio Ferrara, Rudolf M. Mssbauer, World Scientific (2007), ISBN 9812700188, 9789812700186.
- (19) J. A. Maxin, V. E. Mayes and D. V. Nanopoulos, Phys. Rev. D 79 066010 (2009) [arXiv:0809.3200 [hep-ph]].
- (20) R. Blumenhagen, B. Körs, D. Lüst and T. Ott, Nucl. Phys. B 616, 3 (2001) [arXiv:hep-th/0107138].
- (21) M. Cvetič, P. Langacker and G. Shiu, Phys. Rev. D 66, 066004 (2002); Nucl. Phys. B 642, 139 (2002).
- (22) D. Cremades, L. E. Ibáñez and F. Marchesano, JHEP 0207, 009 (2002) [arXiv:hep-th/0201205].
- (23) G. Shiu and S. H. H. Tye, Phys. Rev. D 58, 106007 (1998) [arXiv:hep-th/9805157].
- (24) D. Lüst and S. Stieberger, [arXiv:hep-th/0302221].
- (25) I. Antoniadis, E. Kiritsis and T. N. Tomaras, Phys. Lett. B 486, 186 (2000) [arXiv:hep-ph/0004214]; R. Blumenhagen, D. Lust and S. Stieberger, JHEP 0307, 036 (2003) [arXiv:hep-th/0305146].
- (26) D. Cremades, L. E. Ibáñez and F. Marchesano, JHEP 0307, 038 (2003) [arXiv:hep-th/0302105].
- (27) M. Cvetič and I. Papadimitriou, Phys. Rev. D 68, 046001 (2003) [Erratum-ibid. D 70, 029903 (2004)] [arXiv:hep-th/0303083].
- (28) D. Lüst, P. Mayr, R. Richter and S. Stieberger, Nucl. Phys. B 696, 205 (2004) [arXiv:hep-th/0404134].
- (29) J. F. G. Cascales and A. M. Uranga, JHEP 0305, 011 (2003).
- (30) F. Marchesano and G. Shiu, Phys. Rev. D 71, 011701 (2005); JHEP 0411, 041 (2004).
- (31) M. Cvetič and T. Liu, Phys. Lett. B 610, 122 (2005).
- (32) M. Cvetič, T. Li and T. Liu, Phys. Rev. D 71, 106008 (2005).
- (33) J. Kumar and J. D. Wells, JHEP 0509, 067 (2005).
- (34) C.-M. Chen, V. E. Mayes and D. V. Nanopoulos, Phys. Lett. B 633, 618 (2006).
- (35) R. Blumenhagen, M. Cvetic, F. Marchesano and G. Shiu, JHEP 0503, 050 (2005) [arXiv:hep-th/0502095].
- (36) Y. Kawamura, T. Kobayashi and T. Komatsu, Phys. Lett. B 400, 284 (1997) [arXiv:hep-ph/9609462].
- (37) A. Brignole, L. E. Ibanez and C. Munoz, Nucl. Phys. B 422, 125 (1994) [Erratum-ibid. B 436, 747 (1995)] [arXiv:hep-ph/9308271]; [arXiv:hep-ph/9707209].
- (38) G. Belanger, F. Boudjema, A. Pukhov and A. Semenov, Comput. Phys. Commun. 176, 367 (2007) [arXiv:hep-ph/0607059]; Comput. Phys. Commun. 174, 577 (2006) [arXiv:hep-ph/0405253]; Comput. Phys. Commun. 149, 103 (2002) [arXiv:hep-ph/0112278].
- (39) A. Djouadi, J. L. Kneur and G. Moultaka, Comput. Phys. Commun. 176, 426 (2007) [arXiv:hep-ph/0211331].
- (40) Tevatron Electroweak Working Group and CDF Collaboration and D0 Collab, [arXiv:0808.1089 [hep-ex]].
- (41) G. Hinshaw et al. [WMAP Collaboration], Astrophys. J. Suppl. 180, 225 (2009) [arXiv:0803.0732 [astro-ph]].
- (42) D. N. Spergel et al. [WMAP Collaboration], Astrophys. J. Suppl. 148, 175 (2003) [arXiv:astro-ph/0302209]; Astrophys. J. Suppl. 170, 377 (2007) [arXiv:astro-ph/0603449].
- (43) I. Antoniadis, C. Bachas, J. R. Ellis and D. V. Nanopoulos, Phys. Lett. B 211, 393 (1988); Nucl. Phys. B 328, 117 (1989); Phys. Lett. B 257, 278 (1991); J. R. Ellis, N. E. Mavromatos and D. V. Nanopoulos, Lectures given at International Workshop on Recent Advances in the Superworld, Woodlands, TX, 13-16 Apr 1993, Published in Woodlands Superworld 1993:3-26 (QCD161:I966:1993) [arXiv:hep-th/9311148]; J. R. Ellis, N. E. Mavromatos and D. V. Nanopoulos, Mod. Phys. Lett. A 10, 1685 (1995) [arXiv:hep-th/9503162]; Phys. Lett. B 619, 17 (2005) [arXiv:hep-th/0412240]; D. V. Nanopoulos and D. Xie, Phys. Rev. D 78, 044038 (2008) [arXiv:0710.2312 [hep-th]].
- (44) A. B. Lahanas, N. E. Mavromatos and D. V. Nanopoulos, PMC Phys. A 1, 2 (2007) [arXiv:hep-ph/0608153]; Phys. Lett. B 649, 83 (2007) [arXiv:hep-ph/0612152].
- (45) B. Dutta, A. Gurrola, T. Kamon, A. Krislock, A. B. Lahanas, N. E. Mavromatos and D. V. Nanopoulos, [arXiv:0808.1372 [hep-ph]].
- (46) E. Barberio et al. [Heavy Flavor Averaging Group (HFAG) Collaboration], [arXiv:0704.3575 [hep-ex]].
- (47) M. Misiak et al., Phys. Rev. Lett. 98, 022002 (2007) [arXiv:hep-ph/0609232].
- (48) G. W. Bennett et al. [Muon g-2 Collaboration], Phys. Rev. Lett. 92, 161802 (2004) [arXiv:hep-ex/0401008].
- (49) T. Aaltonen et al. [CDF Collaboration], Phys. Rev. Lett. 100, 101802 (2008) [arXiv:0712.1708 [hep-ex]].
- (50) R. Barate et al. [LEP Working Group for Higgs boson searches and ALEPH Collaboration], Phys. Lett. B 565, 61 (2003) [arXiv:hep-ex/0306033]; W. M. Yao et al (Particle Data Group), J. Phys. G 33, 1 (2006).
- (51) J. Maxin, V. E. Mayes, and D. V. Nanopoulos, In preparation
- (52) G. Belanger, F. Boudjema, A. Pukhov and A. Semenov, [arXiv:0803.2360 [hep-ph]].
- (53) V. N. Lebedenko et al., [arXiv:0812.1150 [astro-ph]].
- (54) J. Angle et al. [XENON Collaboration], Phys. Rev. Lett. 100, 021303 (2008) [arXiv:0706.0039 [astro-ph]].
- (55) Z. Ahmed et al. [CDMS Collaboration], Phys. Rev. Lett. 102, 011301 (2009) [arXiv:0802.3530 [astro-ph]].
- (56) R. W. Schnee et al. [The SuperCDMS Collaboration], [arXiv:astro-ph/0502435].
- (57) E. Aprile [The XENON Collaboration], [arXiv:astro-ph/0502279].
- (58) E. Behnke et al, Science 319, 933 (2008)
- (59) G. J. Alner et al, Phys. Lett. B 616, 17 (2005)
- (60) H. S. Lee. et al. [KIMS Collaboration], Phys. Rev. Lett. 99, 091301 (2007) [arXiv:0704.0423 [astro-ph]].
- (61) S. Desai et al. [Super-Kamiokande Collaboration], Phys. Rev. D 70, 083523 (2004) [Erratum-ibid. D 70, 109901 (2004)] [arXiv:hep-ex/0404025].
- (62) A. Morselli, A. Lionetto, A. Cesarini, F. Fucito and P. Ullio [GLAST Collaboration], Nucl. Phys. Proc. Suppl. 113, 213 (2002) [arXiv:astro-ph/0211327].