Response of mica to weakly interacting massive particles

Engel, J.; Ressell, M. T.; Towner, I.S.; Ormand, W. E.

doi:10.1103/physrevc.52.2216

Cited by 54 publications

(113 citation statements)

References 32 publications

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“…This is due to the fact that most of the Cl 2 3 total nuclear spin is contributed by the nucleons' orbital angular momenta. Since such phenomenon also occurs with 39 K [22], it should reasonably occur with 37 Cl, which has the same neutron number as 39 K. 35 Cl, 37 Cl and 39 K are "nearby" isotopes with low gyromagnetic ratio. The fact that the single nucleon spin gyromagnetic ratios are higher than the corresponding orbital gyromagnetic ratios indicates high orbital angular momenta, both for the proton and the neutron group.…”

Section: Discussionmentioning

confidence: 99%

Model-independent limits from spin-dependent WIMP dark matter experiments

Giuliani¹,

Girard

2005

Phys. Rev. D

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Spin-dependent WIMP searches have traditionally presented results within an odd group approximation and by suppressing one of the spin-dependent interaction cross sections. We here elaborate on a modelindependent analysis in which spin-dependent interactions with both protons and neutrons are simultaneously considered. Within this approach, equivalent current limits on the WIMP-nucleon interaction at WIMP mass of 50 GeV/c 2 are either p 0.7 pb, n 0.2 pb or |a p | 0.4, |a n | 0.7 depending on the choice of cross section or coupling strength representation. These limits become less restrictive for either larger or smaller masses; they are less restrictive than those from the traditional odd group approximation regardless of WIMP mass. Combination of experimental results are seen to produce significantly more restrictive limits than those obtained from any single experiment. Experiments traditionally considered spin-independent are moreover found to severely limit the spin-dependent phase space. The extension of this analysis to the case of positive signal experiments is explored. PACS numbers: 95.35.+d;14.80.Ly;

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Section: Discussionmentioning

confidence: 99%

Model-independent limits from spin-dependent WIMP dark matter experiments

Giuliani¹,

Girard

2005

Phys. Rev. D

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“…The cross sections at zero momentum transfer show strong dependence on the nuclear structure of the ground state [26][27][28].…”

Section: Approach To Our Calculationsmentioning

confidence: 99%

“…The relic neutralinos in the halo of our Galaxy have a mean velocity of v ≃ 300 km/s = 10 −3 c. When the product q max R ≪ 1, where R is the nuclear radius and q max = 2µ A v is the maximum momentum transfer in the χ-A scattering, the matrix element for the SD χ-A scattering reduces to a very simple form (zero momentum transfer limit) [26,27]:…”

Section: Approach To Our Calculationsmentioning

confidence: 99%

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Dark matter search after DAMA withG73e

Bednyakov

Klapdor‐Kleingrothaus²

2004

Phys. Rev. D

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The Weakly Interacting Massive Particle (WIMP) is one of the main candidates for the relic dark matter (DM). In the effective low-energy minimal supersymmetric standard model (effMSSM) the neutralino-nucleon spin and scalar cross sections in the low-mass regime were calculated. The calculated cross sections are compared with almost all experimental currently available exclusion curves for spin-dependent WIMP-proton and WIMP-neutron cross sections. It is demonstrated that in general about two-orders-of-magnitude improvement of the current DM experiment sensitivities is needed to reach the (effMSSM) SUSY predictions. At the current level of accuracy it looks reasonable to safely neglect sub-dominant spin WIMP-nucleon contributions analyzing the data from spin-non-zero targets. To avoid misleading discrepancies between data and SUSY calculations it is, however, preferable to use a mixed spin-scalar coupling approach. This approach is applied to estimate future prospects of experiments with the odd-neutron high-spin isotope 73 Ge. It is noticed that the DAMA evidence favors the light Higgs sector in the effMSSM, a high event rate in a 73 Ge detector and relatively high upgoing muon fluxes from relic neutralino annihilations in the Earth and the Sun.

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“…Assuming q max R ≪ 1, where R is the nuclear radius and q max = 2µ A v is the maximum of the momentum transfer in the process of the χA scattering, the spin-dependent matrix element takes a simple form (zero momentum transfer limit) [77,78] …”

Section: Appendixmentioning

confidence: 99%

One needs positive signatures for detection of Dark Matter

Bednyakov

2013

Phys. Part. Nuclei

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One believes there is huge amount of Dark Matter particles in our Galaxy which manifest themselves only gravitationally. There is a big challenge to prove their existence in a laboratory experiment. To this end it is not sufficient to fight only for the best exclusion curve, one has to see an annual recoil spectrum modulation -the only available positive direct dark matter detection signature. A necessity to measure the recoil spectra is stressed. 95.35.+d, 14.80.Ly, 12.60.Jv Galactic Dark Matter (DM) particles do not emit (or reflect) any detectable electromagnetic radiation and manifest themselves only gravitationally by affecting other astrophysical objects.According to the estimates based on a detailed model of our Galaxy [1] the local density of DM (nearby the solar system) amounts to about ρ (see also recent reviews [2,3]). The local flux of DM particles χ is expected to be Φ DM local ≃ 100 GeV m χ · 10 5 cm −2 s −1 , where m χ is the DM particle mass. This value is often considered as a promising basis for direct laboratory dark matter search experiments.The problem of the DM in the Universe is a challenge for modern physics and experimental technology. To solve the problem, i.e. at least to detect the DM particles, one simultaneously needs to apply the front-end knowledge of modern Particle Physics, Astrophysics, Cosmology and Nuclear Physics and to develop and use over long time extremely high-sensitive experimental setups and complex data analysis methods (see, for example, recent discussion in [4]).Weakly Interacting Massive Particles (WIMPs) are among the most popular candidates for the relic DM. These particles are non-baryonic and there is no room for them in the StandardModel of particle physics (SM). The lightest supersymmetric (SUSY) particle (LSP), neutralino (being massive, neutral and stable), is currently often assumed to be a favorite WIMP dark matter particle.The nuclear recoil energy due to elastic WIMP-nucleus scattering is the main quantity to be measured by a terrestrial detector in direct DM detection laboratory experiments [5]. Detection of the very rare events of such WIMP interactions is a quite complicated task because of very weak WIMP coupling with ordinary matter. The rates expected in the SUSY models range 2 from 10 to 10 −7 events per kilogram detector material a day [6][7][8][9][10][11][12][13]. Moreover, for WIMP masses between a few GeV/c 2 and 1 TeV/c 2 , the energy deposited by the recoil nucleus is less than 100 keV. Therefore, in order to be able to detect a WIMP, an experiment with a low-energy threshold and an extremely low radioactive background is required. Furthermore, to certainly detect a WIMP one has to unambiguously register some positive signature of WIMP-nucleus interactions (directional recoil or annual signal modulation) [7,14]. This means one has to perform a stable measurement with a detector of large target mass during 3-5 years under extremely low radioactive background conditions. There are also some other complications discussed recently in [2,4]...

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Response of mica to weakly interacting massive particles

Cited by 54 publications

References 32 publications

Model-independent limits from spin-dependent WIMP dark matter experiments

Model-independent limits from spin-dependent WIMP dark matter experiments

Dark matter search after DAMA withG73e

One needs positive signatures for detection of Dark Matter

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