Stringy WIMP Detection and Annihilation
Abstract
ABSTRACT
We calculate the direct dark matter detection spinindependent and proton spindependent crosssections for a semirealistic intersecting 6brane model. The crosssections 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 6brane 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 gammaray flux resulting from neutralino annihilation for the 6brane model and compare the flux to the projected sensitivity of the Fermi Gammaray Space Telescope. Finally, we compute the direct and indirect detection crosssections as well as the gammaray flux resulting from WIMP annihilations for the oneparameter model for comparison, where the oneparameter 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.
ACT0509, MIFP0917
I Introduction
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 Rparity 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 gammarays from WIMP annihilation is the process , where two gammarays are produced directly from a WIMP annihilation, and another is . Analyses of direct detection crosssections and gammaray 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 Dbrane 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 supersymmetrybreaking soft terms for intersecting Dbrane models are in general nonuniversal Kors:2003wf (). Despite substantial progress in constructing such models, most supersymmetric Dbrane 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 6brane 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 treelevel and it is also possible to obtain the correct Yukawa mass matrices for both up and downtype quarks and leptons for specific values of the moduli VEVs Chen:2007px () Chen:2007zu (). Furthermore, the softsupersymmetry 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 openstring moduli associated with Dbrane 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 6brane model for varying cases of gravitino masses and tan. The spinindependent crosssections are computed and plotted against the current dark matter detection experiment constraints. Furthermore, we present the proton spindependent crosssections, whereas the computed neutron spindependent crosssections only vary slightly from those of the proton, so the neutron crosssections are not shown. The gammaray flux resulting from neutralino annihilations in the galactic halo for the 6brane 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 spinindependent and spindependent crosssections for the socalled oneparameter model Lopez:1993rm (); Lopez:1994fz (); Lopez:1995hg (); Maxin:2008kp (), including the gammaray flux. The oneparameter 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 noscale supergravity models, generically and , thus the number of free parameters is reduced to two, and tan. Adopting a strict noscale framework, one can also fix the parameter as , and hence we are led to a oneparameter model where all of the soft terms may be fixed in terms of . Therefore, the oneparameter model represents a suitable case with which to compare the intersecting 6brane model with nonuniversal soft supersymmetry breaking terms.
Ii LowEnergy Effective Action
In this section, we give a background discussion for the more technicallyminded reader which describes the way in which the supersymmetry breaking soft terms are calculated for intersecting brane models. In recent years, intersecting Dbrane models have provided an exciting approach toward constructing semirealistic vacua. To summarize, D6branes (in Type IIA) fill threedimensional Minkowski space and wrap 3cycles in the compactified manifold, with a stack of branes having a gauge group (or in the case of ) in its world volume. The 3cycles wrapped by the Dbranes 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 3cycles intersect. Due to orientifolding, for every stack of D6branes we must also introduce its orientifold images. Thus, the D6branes 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 RamondRamond tadpole cancellation and to have a spectrum with supersymmetry.
To discuss the lowenergy phenomenology we start from the lowenergy effective action. From the effective scalar potential it is possible to study the stability Blumenhagen:2001te (), the treelevel 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 softSUSY 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 3form 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 D6brane wrapping a calibrated threecycle is given by (see Blumenhagen:2006ci () for a detailed discussion and explanation of the notation)
(1) 
In terms of the threecycle wrapped by the stack of branes, we have
(2) 
where and are the wrapping numbers of the Dbranes on the th twotorus, from which it follows that
(3) 
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
(4) 
and is the fourdimensional dilaton. To second order in the string matter fields, the K\a”ahler potential is given by
(5)  
The untwisted moduli , are light, nonchiral scalars from the field theory point of view, associated with the Dbrane 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 Dbranes 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:

, ,
(6) 
, ,
(7)
For branes which are parallel on at least one torus, giving rise to nonchiral matter in bifundamental representations (for example, the Higgs doublets), the K\a”ahler metric is
(8) 
The superpotential is given by
(9) 
while the minimum of the F part of the treelevel supergravity scalar potential is given by
(10) 
where and , is inverse of , and the auxiliary fields are given by
(11) 
Supersymmetry is broken when some of the Fterms 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
(12) 
which we will take to be 500 GeV and 700 GeV in the following. The normalized gaugino mass parameters, scalar masssquared parameters, and trilinear parameters respectively may be given in terms of the K\a”ahler potential, the gauge kinetic function, and the superpotential as
(13)  
where is the K\a”ahler metric appropriate for branes which are parallel on at least one torus, i.e. involving nonchiral 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 lowenergy 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 worldsheet instantons and are proportional to , where is the worldsheet 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 openstring moduli. This ensures that the Yukawa couplings present in the soft terms do not depend on either the complexstructure moduli or dilaton (in the supergravity basis). Thus, the Yukawa couplings will not affect the lowenergy 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 ():
(14) 
The factors and are the CP violating phases of the moduli, while the constant is given by
(15) 
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 umoduli 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 5year 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 CPeven 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 crosssections and indirect detection gammaray 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 nonuniversal 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 spinindependent (SI) part and a spindependent(SD) part, where the SI (scalar) interactions are primarily the consequence of elastic collisions with heavy nuclei. First, we consider the SI crosssections for an intersecting 6brane model, then study the SD interactions.
Both the direct detection crosssections and the gammaray 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 crosssections for an intersecting 6brane model. The crosssections 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 ZeplinIII 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 Xenon1 Ton Aprile:2005mz () experiments. Only for = 500 GeV and tan = 10 are the crosssections 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 Xenon1 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 crosssection than the WMAP regions. The dark matter density is inversely proportional to the annihilation crosssection , so one expects the points with a higher to possess a smaller annihilation crosssection, as depicted in Fig. 2.
The proton SD crosssections are shown in Fig. 3. The format of the SD charts is similar to the SI charts. For comparison of the intersecting 6brane model crosssections 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 crosssections (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 crosssections were slightly larger, and the shape of the SD patterns is essentially identical to the SI patterns. None of the intersecting 6brane 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 crosssection than the WMAP points.
V Indirect Dark Matter Detection
Indirect detection experiments search for high energy neutrinos, gammarays, positrons, and antiprotons 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 gammarays in the galactic core or halo. The gammaray flux for the intersecting 6brane 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 gammarays in the galactic core and halo are and . Hence, the flux of gammarays is directly dependent upon the annihilation crosssection. Fig. 2 and Fig. 3 show and we have explained that the SSC points have a smaller annihilation crosssection. Consequently, we expect the SSC points to also exhibit a smaller gammaray flux , and accordingly, this is illustrated in Fig. 4.
It is an intriguing question as to how a model with nonuniversal softsupersymmetry breaking terms, such as an intersecting 6brane model, compares to a model with universal softsupersymmetry breaking terms, for example, mSUGRA. The oneparameter model (OPM) Lopez:1993rm (); Lopez:1994fz (); Lopez:1995hg (); Maxin:2008kp () is a highly constrained small subset of mSUGRA, where all the softsupersymmetry breaking terms may be fixed in terms of the gaugino mass . The OPM has universal softsupersymmetry breaking terms, so it is ideal to compare to the 6brane 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 6brane model. For the same WIMP mass, the WMAP spectra have a larger annihilation crosssection, and hence, gammaray flux than the SSC points, due to the fact that in the WMAP region, we are not allowing for the (10) dilution factor to .
Vi Conclusion
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 softsupersymmetry breaking terms such as mSUGRA. Furthermore, the Fermi Gammaray 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 semirealistic string models. To this end, we began an investigation of the experimental detection parameters for a particular stringderived 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 6brane 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 spinindependent and proton spindependent crosssections. 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 crosssections, thus crosssections for SSC are smaller than those of WMAP. Additionally, we illustrated the galactic gammaray flux for this model resulting from neutralino annihilations. We discover that most of the regions of the 6brane model allowed parameter space will be within the sensitivity of the Fermi telescope.
Vii Acknowledgments
This research was supported in part by the MitchellHeep Chair in High Energy Physics (CMC), by the CambridgeMitchell Collaboration in Theoretical Cosmology, and by the DOE grant DEFG0395Er40917.
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