Large-scale nuclear structure calculations for spin-dependent WIMP scattering with chiral effective field theory currents

By P. Klos, J. Men'endez, D. Gazit, A. Schwenk. 2013

156 citations recorded by the source corpus.

We perform state-of-the-art large-scale shell-model calculations of the structure factors for elastic spin-dependent WIMP scattering off 129,131Xe, 127I, 73Ge, 19F, 23Na, 27Al, and 29Si. This comprehensive survey covers the non-zero-spin nuclei relevant to direct dark matter detection. We include a pedagogical presentation of the formalism necessary to describe elastic and inelastic WIMP-nucleus scattering. The valence spaces and nuclear interactions employed have been previously used in nuclear structure calculations for these mass regions and yield a good spectroscopic description of these isotopes. We use spin-dependent WIMP-nucleus currents based on chiral effective field theory (EFT) at the one-body level and including the leading long-range two-body currents due to pion exchange, which are predicted in chiral EFT. Results for all structure factors are provided with theoretical error bands due to the nuclear uncertainties of WIMP currents in nuclei.

Subfields: Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/75cf0306c5d65d2be61761127e39fd32733e946e

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In Nuclear and High Energy Physics

Citations in the corpus

Constraining dark sectors with monojets and dijets (2015, methodology): “We use the spin structure functions from [52] and the same limitsetting procedure as described in [53] to determine the parameter region excluded at 95%”
Dark matter direct-detection experiments (2015, methodology): “New calculations performed in [116] use chiral effective-field theory currents to determine the couplings of WIMPs to nucleons”
Characterising dark matter searches at colliders and direct detection experiments: vector mediators (2014, unknown): “where μnχ is the DM-nucleon reduced mass, A ≈ 131 is the atomic number of xenon, F (ER) is the Helm nuclear form factor [92], S(ER) is the spin structure function [93], J is the nucleus spin, the sum extends over all isotopes with non-zero spin and fi is the fractional abundance of the ith isotope w”
Extended gamma-ray emission from Coy Dark Matter (2014, background): “2) leads to a spin-dependent interaction; for dark matter with speed v, we find that the differential scattering cross-section to scatter of a nucleus of mass mN with spin JN and spin structure function SA(q) [98] is”
Form factors for dark matter capture by the Sun in effective theories (2015, background): “Two-body interactions have also been included in [39, 40] in an investigation of spin-dependent dark matter-nucleus currents.”