Direct detection of dark matter in the minimal supersymmetric standard model with non-universal Higgs boson masses

Abstract

We calculate dark matter scattering rates in the minimal supersymmetric extension of the standard model ͑MSSM͒, allowing the soft supersymmetry-breaking masses of the Higgs multiplets, m 1,2 , to be nonuniversal ͑NUHM͒. Compared with the constrained MSSM ͑CMSSM͒ in which m 1,2 are required to be equal to the soft supersymmetry-breaking masses m 0 of the squark and slepton masses, we find that the elastic scattering cross sections may be up to two orders of magnitude larger than values in the CMSSM for similar lightest supersymmetric particle masses. We find the following preferred ranges for the spin-independent cross section, 10 Ϫ6 pbտ SI տ10 Ϫ10 pb, and, for the spin-dependent cross section, 10 Ϫ3 pbտ SD , with the lower bound on SI dependent on using the putative constraint from the muon anomalous magnetic moment. We stress the importance of incorporating accelerator and dark matter constraints in restricting the NUHM parameter space, and also of requiring that no undesirable vacuum appear below the grand unified theory ͑GUT͒ scale. In particular, values of the spin-independent cross section another order of magnitude larger would appear to be allowed, for small tan ␤, if the GUT vacuum stability requirement were relaxed, and much lower cross-section values would be permitted if the muon anomalous magnetic moment constraint were dropped.

Correlation between direct dark matter detection andBr(Bs→μμ)with a large phase ofBsDutta1, Mimura2, Santoso3 2009Phys. Rev. DSelf Cite3010View full textAdd to dashboardCite

“…Therefore, m A is also important for the proton-neutralino elastic scattering cross-section, and this is particularly the case for models with non-universal Higgs masses [32,33,34]. Thus, there is a correlation between the direct detection of the Milky Way dark matter and Br(B s → µµ) [17].…”

Electric dipole moments in the MSSM at large tanβ

“…We use this more conservative range in addition to that suggested by the recent WMAP data [72] (0.094 ≤ Ω χ h 2 ≤ 0.129) for clarity in the figures. The effect of the WMAP densities in the CMSSM was discussed in [73] and in the NUHM in [74]. We also require that the lightest supersymmetric particle (LSP) be a neutralino.…”

Dark matter search after DAMA withG73e

“…To obtain as much as general predictions it appeared more convenient to work within a phenomenological SUSY model whose parameters are defined directly at the electroweak scale, relaxing completely constraints following from any unification assumption as for example in [44][45][46][47][48][49], and which is called an effective scheme of MSSM (effMSSM) in [50], and later by some people low-energy effective supersymmetric theory (LEEST) in [5,6]. In our previous calculations in effMSSM [4, 11, 18-20, 44, 51-54] we have adopted some effective scheme (with non-universal scalar masses and with non-universal gaugino soft masses) which lead to large values for direct detection rates of DM neutralinos.…”

“…From (7) one can also see that contrary to the spin-independent case (6) there is no, in general, factorization of the nuclear structure for σ A SD (0). Both proton S A p and neutron S A n spin contributions simultaneously enter into formula (7) for the SD WIMP-nucleus cross section σ A SD (0).…”