Progress on the ARIADNE Axion Experiment

Fosbinder-Elkins, H.; Lohmeyer, Chloe; Dargert, J.; Cunningham, M.; Harkness, M.; Levenson-Falk, E. M.; Mumford, S.; Kapitulnik, A.; Arvanitaki, Asimina; Lee, I.; Smith, E.; Wiesman, E.; Shortino, J.; Long, J. C.; Snow, W. M.; Liu, C.-Y.; Shin, Yunchang; Semertzidis, Yannis K.; Lee, Y.-H.

doi:10.1007/978-3-319-92726-8_18

Cited by 36 publications

(29 citation statements)

References 25 publications

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“…In that case, the expected sensitivity of such experiments must be re-evaluated to take this clustering into account. Experiments such as ARIADNE [163,164], Halo spectrum for QCD axion DM in terms of scale mass Ms and scale density ρs for various values of decay constant fa. The predicted CDM halo spectrum is also shown, although the scales here are far smaller than any that have yet been measured.…”

Section: Qcd Axionmentioning

confidence: 99%

Large-misalignment mechanism for the formation of compact axion structures: Signatures from the QCD axion to fuzzy dark matter

et al. 2020

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Axions are some of the best motivated particles beyond the Standard Model. We show how the attractive self-interactions of dark matter (DM) axions over a broad range of masses, from 10 −22 eV to 10 7 GeV, can lead to nongravitational growth of density fluctuations and the formation of bound objects. This structure formation enhancement is driven by parametric resonance when the initial field misalignment is large, and it affects axion density perturbations on length scales of order the Hubble horizon when the axion field starts oscillating, deep inside the radiation-dominated era. This effect can turn an otherwise nearly scale-invariant spectrum of adiabatic perturbations into one that has a spike at the aforementioned scales, producing objects ranging from dense DM halos to scalar-field configurations such as solitons and oscillons. We call this class of cosmological scenarios for axion DM production "the large-misalignment mechanism."We explore observational consequences of this mechanism for axions with masses up to 10 eV. For axions heavier than 10 −5 eV, the compact axion halos are numerous enough to significantly impact Earth-bound direct detection experiments, yielding intermittent but coherent signals with repetition rates exceeding one per decade and crossing times less than a day. These episodic increases in the axion density and kinematic coherence suggest new approaches for axion DM searches, including for the QCD axion. Dense structures made up of axions from 10 −22 eV to 10 −5 eV are detectable through gravitational lensing searches, and their gravitational interactions can also perturb baryonic structures and alter star formation. At very high misalignment amplitudes, the axion field can undergo self-interaction-induced implosions long before matter-radiation equality, producing potentially-detectable low-frequency stochastic gravitational waves.

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Section: Qcd Axionmentioning

confidence: 99%

Large-misalignment mechanism for the formation of compact axion structures: Signatures from the QCD axion to fuzzy dark matter

et al. 2020

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“…An important conclusion of this work is that a tiny fraction ∼ 10 −17 of the number of axions emitted within the Earth will be lowvelocity (v ≤ v esc ), and thus will be trapped by the Earth. Over 4.5 billion years of accumulation these bound axions may become dense enough for detection by instruments such as ADMX and ADMX-HF [37], upgraded CAST [38], ORPHEUS [39], MADMAX [40], ORGAN [41,42], CULTASK [43], ARIADNE [44], CASPEr [45], ABRA-CADABRA [46], QUAX [47], X3 [48], DM Radio [49], TOORAD [50], axion plasma haloscope [51].…”

Section: Introductionmentioning

confidence: 99%

Gravitationally trapped axions on the Earth

et al. 2019

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We advocate for the idea that there is a fundamentally new mechanism for axion production on Earth, as recently suggested in [1,2]. We specifically focus on production of axions within Earth, with low velocities such that they will be trapped in the gravitational field. Our computations are based on the so-called Axion Quark Nugget (AQN) dark matter model, which was originally invented to explain the similarity of the dark and visible cosmological matter densities. This occurs in the model irrespective of the axion mass ma or initial misalignment angle θ0. Annihilation of antimatter AQNs with visible matter inevitably produce axions when AQNs hit Earth. The emission rate of axions with velocities below escape velocity is very tiny compared to the overall emission, however these axions will be accumulated over the 4.5 billion year life time of the Earth, which greatly enhances the discovery potential. We perform numerical simulations with a realistically modeled incoming AQN velocity and mass distribution, and explore how AQNs interact as they travel through the interior of the Earth. We use this to estimate the axion flux on the surface of the Earth, the velocity-spectral features of trapped axions, the typical annihilation pattern of AQN, and the density profile of the axion halo around the Earth. Knowledge of these properties is necessary to make predictions for the observability of trapped axions using CAST, ADMX, MADMAX, CULTASK, ORPHEUS, ARIADNE, CASPEr, ABRACADABRA, QUAX, ORGAN, TOORAD, DM Radio.2 In particular, a first-order phase transition is not required as the axion domain wall plays the role of the squeezer. Another problem with [34,35] is that nuggets will likely evaporate on a Hubble time-scale even. For the AQN model this argument is not applicable because the vacuum-ground-state energies inside (color-superconducting phase) and outside (hadronic phase) the nugget are drastically different. Therefore, these two systems can arXiv:1905.00022v2 [astro-ph.CO]

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“…We show how new physics at the 1-10 TeV scale can raise T ws so that the axion can constitute a subdominant or correct amount of dark matter. In addition to new heavy states, axiogenesis also favors a small decay constant which is accessible to many axion haloscope and helioscope experiments [74][75][76][77][78][79][80][81][82][83][84][85][86]. The evolution of the PQ breaking field reveals nonstandard cosmological eras, which alone may have profound implications for other aspects of cosmology.…”

mentioning

confidence: 99%

Axiogenesis

2020

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We propose a mechanism called axiogenesis where the cosmological excess of baryons over antibaryons is generated from the rotation of the QCD axion. The Peccei-Quinn (PQ) symmetry may be explicitly broken in the early universe, inducing the rotation of a PQ charged scalar field. The rotation corresponds to the asymmetry of the PQ charge, which is converted into the baryon asymmetry via QCD and electroweak sphaleron transitions. In the concrete model we explore, interesting phenomenology arises due to the prediction of a small decay constant and the connections with new physics at the LHC and future colliders and with axion dark matter.Introduction.-One of the goals of fundamental physics is to understand the origin of the Universe. For this purpose, the Standard Model (SM) of particle physics needs an extension to explain the cosmological excess of matter over antimatter. Mechanisms to generate the baryon asymmetry have been intensively studied in the literature under the name of baryogenesis [1][2][3][4][5][6][7][8].The SM also needs an extension to explain the smallness of CP violation in QCD [9] which on theoretical grounds is expected to be large [10]. This is known as the strong CP problem and can be elegantly solved by the Peccei-Quinn (PQ) mechanism [11,12]. The so-called the PQ symmetry is spontaneously broken to yield a pseudo Nambu-Goldstone boson, the axion [13,14]. The PQ symmetry is explicitly broken by the quantum effects of QCD of the Adler-Bell-Jeckiw type [15,16]. The quantum effects give a potential to the axion and drive the axion field value to the point where CP symmetry is restored, solving the strong CP problem. The axion is also a dark matter candidate [17][18][19], which makes the PQ mechanism even more attractive.We discover that when the PQ mechanism is introduced into the SM, the baryon (B) and lepton (L) asymmetries are generated in a wide class of models. We call the following baryogenesis scheme as axiogenesis, which in general includes two main ingredients: 1) an asymmetry of the PQ charge is generated in the early universe as a coherent rotation in the axion direction and 2) the PQ asymmetry is later transferred to the B + L asymmetry via the QCD and electroweak sphaleron transitions. We contrast axiogenesis with other existing baryogenesis models after we introduce a concrete example. (We may convert the B + L asymmetry into the B − L asymmetry by some B − L breaking interaction. The investigation of such a scenario will be considered in a future work [20].)The PQ symmetry is an approximate global symmetry which is explicitly broken by the QCD anomaly. Given that the symmetry is not exact, it is conceivable that the PQ symmetry is significantly broken in the early universe, and the rotation of the axion is induced. In fact, it is expected that quantum gravity does not allow for a global symmetry [21][22][23][24][25] and the PQ symmetry is at best understood as an accidental symmetry explicitly broken by higher dimensional operators [26][27][28][29]. Even when one requires that t...

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Progress on the ARIADNE Axion Experiment

Cited by 36 publications

References 25 publications

Large-misalignment mechanism for the formation of compact axion structures: Signatures from the QCD axion to fuzzy dark matter

Large-misalignment mechanism for the formation of compact axion structures: Signatures from the QCD axion to fuzzy dark matter

Gravitationally trapped axions on the Earth

Axiogenesis

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