Search for dark matter axions with the Orpheus experiment

Rybka, G.; Wagner, A.; Patel, Kunal; Percival, Robert; Ramos, Kathleen J.; Brill, A.

doi:10.1103/physrevd.91.011701

Cited by 118 publications

(141 citation statements)

References 29 publications

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“…This substructure forms immediately after the QCD phase transition as discussed in [3]. The equilibrium of the obtained system has been analyzed in [3] for a specific axion domain wall tension within the observationally allowed window 10 −6 eV ≤ m a ≤ 10 −3 eV consistent with the recent constraints [8][9][10][11][12][13][14][15]. It has been also argued in [3] that the equilibrium is typically achieved when the Fermi pressure inside the nuggets falls into the region when the colour superconductivity (CS) indeed sets in 1 .…”

Section: −1 Amentioning

confidence: 70%

“…Finally, an overall coherent baryon asymmetry in the entire Universe is a result of the strong CP violation due to the fundamental θ parameter in QCD which is assumed to be nonzero at the beginning of the QCD phase transition. This source of strong CP violation is no longer available at the present epoch as a result of the axion dynamics, see original papers [5][6][7] and recent reviews [8][9][10][11][12][13][14][15] on the subject. We highlight the basics ideas of this framework in the present Introduction, while we elaborate on these new crucial elements in details in section III.…”

Section: Introductionmentioning

confidence: 99%

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Axion field and the quark nugget’s formation at the QCD phase transition

2016

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We study a testable dark matter (DM) model outside of the standard WIMP paradigm in which the observed ratio Ω dark Ω visible for visible and dark matter densities finds its natural explanation as a result of their common QCD origin when both types of matter (DM and visible) are formed at the QCD phase transition and both are proportional to ΛQCD. Instead of conventional "baryogenesis" mechanism we advocate a paradigm when the "baryogenesis" is actually a charge separation process which always occur in the presence of the CP odd axion field a(x). In this scenario the global baryon number of the Universe remains zero, while the unobserved anti-baryon charge is hidden in form of heavy nuggets, similar to Witten's strangelets and compromise the DM of the Universe.In the present work we study in great details a possible formation mechanism of such macroscopically large heavy objects. We argue that the nuggets will be inevitably produced during the QCD phase transition as a result of Kibble-Zurek mechanism on formation of the topological defects during a phase transition. Relevant topological defects in our scenario are the closed bubbles made of the NDW = 1 axion domain walls. These bubbles, in general, accrete the baryon (or anti baryon) charge, which eventually result in formation of the nuggets and anti-nuggets carrying a huge baryon (anti-baryon) charge. A typical size and the baryon charge of these macroscopically large objects is mainly determined by the axion mass ma. However, the main consequence of the model, Ω dark ≈ Ω visible is insensitive to the axion mass which may assume any value within the observationally allowed window 10 −6 eV ma 10 −3 eV. We also estimate the baryon to entropy ratio η ≡ nB/nγ ∼ 10 −10 within this scenario. Finally, we comment on implications of these results to the axion search experiments, including microwave cavity and the Orpheus experiments.

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Section: −1 Amentioning

confidence: 70%

Section: Introductionmentioning

confidence: 99%

Axion field and the quark nugget’s formation at the QCD phase transition

2016

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“…The values shift between KSVZ and DFSZ models since the domain wall number N DW = 1 for KSVZ and 6 for DFSZ and m a ≃ 0.62 eV [10 7 GeV/(f a /N DW )]. We also note that a possible ADMX technique of open resonators [98] may allow even lower values of f a to be probed in the future.…”

Section: Resultsmentioning

confidence: 99%

Mixed axion-wino dark matter

et al. 2015

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A variety of supersymmetric models give rise to a split mass spectrum characterized by very heavy scalars but sub-TeV gauginos, usually with a wino-like LSP. Such models predict a thermally-produced underabundance of wino-like WIMP dark matter so that non-thermal DM production mechanisms are necessary. We examine the case where theories with a wino-like LSP are augmented by a Peccei-Quinn sector including an axion-axino-saxion supermultiplet in either the SUSY KSVZ or SUSY DFSZ models and with/without saxion decays to axions/axinos. We show allowed ranges of PQ breaking scale f a for various cases which are generated by solving the necessary coupled Boltzmann equations. We also present results for a model with radiatively-driven naturalness but with a wino-like LSP.

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“…Fortunately, there are a number of running (ADMX [71], HAYSTAC [88], OR-GAN [89]), presently being assembled (CULTASK [72], QUAX [90]), or planned (ABRA-CADABRA [73], KLASH [91], MADMAX [74], ORPHEUS [92]) axion dark matter experiments, which cover a large portion of the mass range of interest for axion dark matter in the pre-inflationary PQ symmetry scenario in Model 2.1, see figure 12. 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.…”

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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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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Search for dark matter axions with the Orpheus experiment

Cited by 118 publications

References 29 publications

Axion field and the quark nugget’s formation at the QCD phase transition

Axion field and the quark nugget’s formation at the QCD phase transition

Mixed axion-wino dark matter

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

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