Resonantly Detecting Axion-Mediated Forces with Nuclear Magnetic Resonance

Arvanitaki, Asimina; Geraci, Andrew

doi:10.1103/physrevlett.113.161801

Cited by 244 publications

(273 citation statements)

References 35 publications

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“…Note that the region in the N DW = 3 case has been derived under the assumption that the PQ symmetry is protected by a discrete symmetry, so that Planck scale suppressed PQ violating operators are allowed at dimension 10 or higher [69]. In the last two lines the projected sensitivities of various experiments are indicated [70][71][72][73][74][75][76][77].…”

Section: Summary and Discussionmentioning

confidence: 99%

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Axion predictions in SO(10) × U(1)PQ models

Ernst

Ringwald

Tamarit

2018

J. High Energ. Phys.

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Non-supersymmetric Grand Unified SO(10) × U(1) PQ models have all the ingredients to solve several fundamental problems of particle physics and cosmologyneutrino masses and mixing, baryogenesis, the non-observation of strong CP violation, dark matter, inflation -in one stroke. The axion -the pseudo Nambu-Goldstone boson arising from the spontaneous breaking of the U(1) PQ Peccei-Quinn symmetry -is the prime dark matter candidate in this setup. We determine the axion mass and the low energy couplings of the axion to the Standard Model particles, in terms of the relevant gauge symmetry breaking scales. We work out the constraints imposed on the latter by gauge coupling unification. We discuss the cosmological and phenomenological implications.

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Section: Summary and Discussionmentioning

confidence: 99%

“…Furthermore, in the meV mass range of interest for the post-inflationary PQ symmetry breaking scenario, the model can be probed by the presently being build fifth force experiment ARIADNE [75] and the proposed helioscope IAXO [76], cf. figure 12.…”

Section: Jhep02(2018)103mentioning

confidence: 99%

Axion predictions in SO(10) × U(1)PQ models

Ernst

Ringwald

Tamarit

2018

J. High Energ. Phys.

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“…All such high f a QCD axions are ruled out. Even if they can exist (by somehow suppressing the fluctuation contribution to the abundance), evading isocurvature bounds will require searches for them to be independent of the DM abundance [52]. In the general, non-QCD, case low f a < H I /2π axions [53] are unaffected by the tensor bound.…”

Section: Introductionmentioning

confidence: 99%

Tensor Interpretation of BICEP2 Results Severely Constrains Axion Dark Matter

et al. 2014

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The recent detection of B-modes by BICEP2 has non-trivial implications for axion dark matter implied by combining the tensor interpretation with isocurvature constraints from Planck. In this paper the measurement is taken as fact, and its implications considered, though further experimental verification is required. In the simplest inflation models r = 0.2 implies HI = 1.1 × 10 14 GeV. If the axion decay constant fa < HI /2π constraints on the dark matter (DM) abundance alone rule out the QCD axion as DM for ma 52χ 6/7 µeV (where χ > 1 accounts for theoretical uncertainty). If fa > HI /2π then vacuum fluctuations of the axion field place conflicting demands on axion DM: isocurvature constraints require a DM abundance which is too small to be reached when the back reaction of fluctuations is included. High fa QCD axions are thus ruled out. Constraints on axionlike particles, as a function of their mass and DM fraction, are also considered. For heavy axions with ma 10 −22 eV we find Ωa/Ω d 10 −3 , with stronger constraints on heavier axions. Lighter axions, however, are allowed and (inflationary) model-independent constraints from the CMB temperature power spectrum and large scale structure are stronger than those implied by tensor modes. −0.05 has profound implications for our understanding of the initial conditions of the universe [2], and points to an inflationary origin for the primordial fluctuations [3][4][5]. The inflaton also drives fluctuations in any other fields present in the primordial epoch and so the measurement of r, which fixes the inflationary energy scale, can powerfully constrain diverse physics. In this work we will discuss the implications for axion dark matter (DM) in the case that the tensor modes are generated during single-field slow-roll inflation (from now on we simply refer to this as 'inflation') by zero-point fluctuations of the graviton. In this work we assume that the measured value of r both holds up to closer scrutiny experimentally, and is taken to be of primordial origin. We relax these assumptions in our closing discussion. We stress that our conclusions are one consequence of taking this measurement at face value, but also that they apply to any detection of r.The scalar amplitude of perturbations generated during inflation is given by [7]

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“…Axions are among the most well motivated of the viable dark-matter candidates, with many theories of beyond the standard model physics including mechanisms that can produce ubiquitous axions and other ultralight bosons with the correct abundance to match the observed dark-matter density [2][3][4][5][6][7][8][9][10][11][12]. The large parameter space where ultralight bosons are good dark-matter candidates has inspired new interest in experimental searches for axion and axionlike searches [13][14][15][16][17][18][19][20][21][22][23][24][25][26][27][28] as well as other types of ultralight bosonic dark matter , with many experiments in progress.…”

Section: Introductionmentioning

confidence: 99%

Spin precession experiments for light axionic dark matter

et al. 2018

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Axionlike particles are promising candidates to make up the dark matter of the Universe, but it is challenging to design experiments that can detect them over their entire allowed mass range. Dark matter in general, and, in particular, axionlike particles and hidden photons, can be as light as roughly 10 −22 eV (∼10 −8 Hz), with astrophysical anomalies providing motivation for the lightest masses ("fuzzy dark matter"). We propose experimental techniques for direct detection of axionlike dark matter in the mass range from roughly 10 −13 eV (∼10 2 Hz) down to the lowest possible masses. In this range, these axionlike particles act as a time-oscillating magnetic field coupling only to spin, inducing effects such as a timeoscillating torque and periodic variations in the spin-precession frequency with the frequency and direction of these effects set by the axion field. We describe how these signals can be measured using existing experimental technology, including torsion pendulums, atomic magnetometers, and atom interferometry. These experiments demonstrate a strong discovery capability, with future iterations of these experiments capable of pushing several orders of magnitude past current astrophysical bounds.

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Resonantly Detecting Axion-Mediated Forces with Nuclear Magnetic Resonance

Cited by 244 publications

References 35 publications

Axion predictions in SO(10) × U(1)PQ models

Axion predictions in SO(10) × U(1)PQ models

Tensor Interpretation of BICEP2 Results Severely Constrains Axion Dark Matter

Spin precession experiments for light axionic dark matter

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