Direct detection of light anapole and magnetic dipole DM

Nobile, Eugenio Del; Gelmini, Graciela B.; Gondolo, Paolo; Huh, Jin Hoe

doi:10.1088/1475-7516/2014/06/002

Cited by 77 publications

(116 citation statements)

References 122 publications

(262 reference statements)

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“…In the absence of unknown form factors, all experimental data can be mapped into v minspace at each DM mass and compared without specifying the nature of the astrophysical distribution or density of DM [39,40]. These "halo-independent" methods have received significant attention [41][42][43][44][45][46][47][48][49][50][51][52][53][54][55][56]. We generalize these methods to cover relativistic scattering as well, where the "halo-independence" here comes from the absence of specific assumptions regarding the local DM density, density profile, velocity distribution, and annihilation source.…”

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confidence: 99%

Direct Detection Phenomenology in Models Where the Products of Dark Matter Annihilation Interact with Nuclei

2015

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We investigate the direct detection phenomenology of a class of dark matter (DM) models in which DM does not directly interact with nuclei, but rather the products of its annihilation do. When these annihilation products are very light compared to the DM mass, the scattering in direct detection experiments is controlled by relativistic kinematics. This results in a distinctive recoil spectrum, a non-standard and or even absent annual modulation, and the ability to probe DM masses as low as a ∼10 MeV. We use current LUX data to show that experimental sensitivity to thermal relic annihilation cross sections has already been reached in a class of models. Moreover, the compatibility of dark matter direct detection experiments can be compared directly in Emin space without making assumptions about DM astrophysics, mass, or scattering form factors. Lastly, when DM has direct couplings to nuclei, the limit from annihilation to relativistic particles in the Sun can be stronger than that of conventional non-relativistic direct detection by more than three orders of magnitude for masses in a 2-7 GeV window.Introduction -While very little is known about Dark Matter (DM), its cosmological abundance is experimentally quite well-determined: Ω CDM h 2 = 0.1199 ± 0.0027 [1]. An appealing framework for understanding the relic abundance of Dark Matter (DM) is thermal freeze-out [2]. Number-changing interactions in the early universe, XX ↔ (SM)SM keep DM in thermal equilibrium with the SM bath, until the rate of these annihilation processes drops below the rate of Hubble expansion. After this point the abundance of DM is essentially fixed at, Ω CDM h 2 0.12 6 × 10 −26 cm 3 s −1 / σ ann v rel , singling out a characteristic annihilation cross section σ ann v rel for thermally produced DM to yield the observed abundance. This scenario is attractive in that it provides a simple and elegant framework for the relic abundance that can be tested in a variety of ways, including direct detection (DD) [3]. However, current constraints from DD rule out many of the simplest models of thermal relic DM, which may indicate a modification of the above picture.In this paper we investigate a modification of thermal DM which alleviates the tension between DD constraints and the thermal relic hypothesis, while making unique predictions for DD. In particular, we take the abundance of DM, X, to be determined by the annihilation process XX ↔ Y Y , where Y is a much lighter dark sector species. The interactions of the dark sector state Y with ordinary nuclei allows for a unique test of the scenario at DD experiments. The resulting DD phenomenology of this class of models is distinctive, owing to the fact that (1) the scattering partner of the nucleus is relativistic, rendering the kinematics of scattering completely different and (2) it is the flux of the scattering partner Y that determines the rate of events at a detector rather than X. Both of these features have novel consequences not considered in the literature of "model-independent" direct detecti...

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confidence: 99%

Direct Detection Phenomenology in Models Where the Products of Dark Matter Annihilation Interact with Nuclei

2015

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“…In applying the s-wave constraints, the dominant mass m f appears as a free parameter in the amplitude in Eq. (13). The resulting lower bound on m f is depicted as the (black) solid curve in Fig.…”

Section: Confronting Constraints On S-wave Annihilationmentioning

confidence: 99%

Anapole dark matter annihilation into photons

Latimer¹

2017

Phys. Rev. D

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In models of anapole dark matter (DM), the DM candidate is a Majorana fermion whose primary interaction with standard model (SM) particles is through an anapole coupling to off-shell photons. As such, at tree-level, anapole DM undergoes p-wave annihilation into SM charged fermions via a virtual photon. But, generally, Majorana fermions are polarizable, coupling to two real photons. This fact admits the possibility that anapole DM can annihilate into two photons in an s-wave process. Using an explicit model, we compute both the tree-level and diphoton contributions to the anapole DM annihilation cross section. Depending on model parameters, the s-wave process can either rival or be dwarfed by the p-wave contribution to the total annihilation cross section. Subjecting the model to astrophysical upper bounds on the s-wave annihilation mode, we rule out the model with large s-wave annihilation.

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“…For the present leptophilic DM model, the relevant scattering of two DM components with the target nucleus is proceeded by the mediation of a virtual photon. As discussed in the literature [70][71][72][73][74][75][76], we first need to identify the relevant effective operators with the DMs coupled to a photon, and then calculate the scattering probability of the DM particles with the target nucleus. Each DM can be viewed as a Majorana particle in the mass eigenstate basis χ i , so that if the scattering does not change the DM component, for the so-called component-conserving scattering, one has to only consider the following two kinds of dimension-six effective operators…”

Section: Direct Dark Matter Detectionsmentioning

confidence: 99%

“…[70], it can be proved that O c 2i = −2O c 1i by using the Chisholm identity, which results in a single kind of the dimension-six operator for the Majorana fermions. This kind of operators can be matched to the electromagnetic anapole moment of each DM component, which further couples to the current from the target nucleus in the non-relativistic limit and realizes the anapole dark matter [70,[74][75][76]. However, besides the above component-conserving interactions, there are also transition interactions induced by the real Yukawa couplings,…”

Section: Direct Dark Matter Detectionsmentioning

confidence: 99%

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X-ray line from the dark transition electric dipole

Geng

Huang

Tsai

2014

J. High Energ. Phys.

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Abstract:We study a two-component dark matter (DM) model in which the two Majorana fermionic DM components with nearly degenerate masses are stabilized by an Z 2 symmetry and interact with the right-handed muon and tau only via real Yukawa couplings, together with an additional Z 2 -odd singly-charged scalar. In this setup, the decay from the heavy DM to the lighter one via the transition electric dipole yields the 3.55 keV X-ray signal observed recently. The Yukawa couplings in the dark sector are assumed to be hierarchical, so that the observed DM relic abundance can be achieved with the leading s-wave amplitudes without a fine-tuning. We also consider the constraints from flavor physics, DM direct detections and collider searches, respectively.

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Direct detection of light anapole and magnetic dipole DM

Cited by 77 publications

References 122 publications

Direct Detection Phenomenology in Models Where the Products of Dark Matter Annihilation Interact with Nuclei

Direct Detection Phenomenology in Models Where the Products of Dark Matter Annihilation Interact with Nuclei

Anapole dark matter annihilation into photons

X-ray line from the dark transition electric dipole

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