New solar axion search using the CERN Axion Solar Telescope with<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:mmultiscripts><mml:mrow><mml:mi>He</mml:mi></mml:mrow><mml:mprescripts/><mml:none/><mml:mrow><mml:mn>4</mml:mn></mml:mrow></mml:mmultiscripts></mml:mrow></mml:math>filling

Arık, M.; Aune, S.; Barth, K.; Белов, А. С.; Bräuninger, H.; Bremer, J.; Burwitz, V.; Cantatore, G.; Carmona, J. M.; Çetin, S. A.; Collar, J. I.; Riva, Enrico Da; Dafní, T.; Davenport, M.; Dermenev, A.; Eleftheriadis, C.; Elías, Nicolás; Fanourakis, G.; Ferrer‐Ribas, E.; Galán, J.; Garcı́a, Juan Antonio; Gardikiotis, A.; Garza, J.G.; Gazis, E. N.; Geralis, T.; Georgiopoulou, E.; Giomataris, I.; Gninenko, S.; Marzoa, M. Gómez; Hasinoff, M.; Hoffmann, D. H. H.; Iguaz, F.J.; Irastorza, I.G.; Jacoby, J.; Jakovčić, K.; Karuza, M.; Kavuk, Mehmet; Krčmar, M.; Kuster, M.; Lakić, B.; Laurent, J.; Liolios, A.; Ljubičić, A.; Luzón, G.; Neff, S.; Niinikoski, T.; Nordt, Annika; Ortega, I.; Papaevangelou, T.; Pivovaroff, M. J.; Raffelt, Georg G.; Rodríguez, A. Soto; Rosu, M.; Ruz, J.; Savvidis, I.; Shilon, I.; Solanki, S. K.; Stewart, L.; Tomás, A.; Vafeiadis, T.; Villar, J.A.; Vogel, Julia K.; Yildiz, S.C.; Zioutas, K.

doi:10.1103/physrevd.92.021101

Cited by 61 publications

(49 citation statements)

References 76 publications

(127 reference statements)

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“…It uses a Large Hadron Collider (LHC) dipole prototype magnet with a magnetic field of up to 9 T over a length of 9.3 m and an aperture of 2 × 15 cm 2 [27], that is able to follow the Sun for ∼3 hours per day using an elevation and azimuth drive. During its 10-year experimental program [25,[28][29][30][31][32], CAST has seen no signal of solar axions, and a number of upper limits on the photon-axion coupling g aγ at the level of 10 −10 GeV −1 for axion masses up to ∼1 eV have been derived. It is the most stringent experimental bound in most of this axion mass range.…”

Section: Micromegas Chambers In the Search For Solar Axionsmentioning

confidence: 99%

Gaseous time projection chambers for rare event detection: results from the T-REX project. II. Dark matter

Irastorza

Aznar

Castel

et al. 2016

J. Cosmol. Astropart. Phys.

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Abstract. As part of the T-REX project, a number of R&D and prototyping activities have been carried out during the last years to explore the applicability of gaseous Time Projection Chambers (TPCs) with Micromesh Gas Structures (Micromegas) in rare event searches like double beta decay, axion research and low-mass WIMP searches. While in the companion paper we focus on double beta decay, in this paper we focus on the results regarding the search for dark matter candidates, both axions and WIMPs.

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Section: Micromegas Chambers In the Search For Solar Axionsmentioning

confidence: 99%

Gaseous time projection chambers for rare event detection: results from the T-REX project. II. Dark matter

Irastorza

Aznar

Castel

et al. 2016

J. Cosmol. Astropart. Phys.

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“…The data analysis follows similar previous analyses of CAST data [14][15][16] . We define an unbinned likelihood function…”

Section: Data Analysis and Resultsmentioning

confidence: 99%

New CAST limit on the axion–photon interaction

2017

Nature Phys

836

709

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Hypothetical low-mass particles, such as axions, provide a compelling explanation for the dark matter in the universe. Such particles are expected to emerge abundantly from the hot interior of stars. To test this prediction, the CERN Axion Solar Telescope (CAST) uses a 9 T refurbished Large Hadron Collider test magnet directed towards the Sun. In the strong magnetic field, solar axions can be converted to X-ray photons which can be recorded by X-ray detectors. In the 2013-2015 run, thanks to low-background detectors and a new X-ray telescope, the signal-to-noise ratio was increased by about a factor of three. Here, we report the best limit on the axion-photon coupling strength (0.66 × 10 −10 GeV −1 at 95% confidence level) set by CAST, which now reaches similar levels to the most restrictive astrophysical bounds.A dvancing the low-energy frontier is a key endeavour in the worldwide quest for particle physics beyond the standard model and in the effort to identify dark matter 1,2 . Nearly massless pseudoscalar bosons, often generically called axions, are particularly promising because they appear in many extensions of the standard model. They can be dark matter in the form of classical field oscillations that were excited in the early universe, notably by the re-alignment mechanism 3 . One particularly well motivated case is the quantum chromodynamics (QCD) axion, the eponym for all such particles. The existence of this new lowmass boson follows from the Peccei-Quinn mechanism as an explanation why QCD is perfectly time-reversal invariant within current experimental precision 3 .Axions were often termed 'invisible' because of their extremely feeble interactions, yet they are the target of a fast-growing international landscape of experiments. Numerous existing and foreseen projects assume that axions are the galactic dark matter and use a variety of techniques that are sensitive to different interaction channels and optimal in different mass ranges 4 . Independently of the dark-matter assumption, one can search for new forces mediated by these low-mass bosons 5 or the back-reaction on spinning black holes (superradiance) 6 . Stellar energy-loss arguments provide restrictive limits that can guide experimental efforts, and in some cases may even suggest new loss channels 3,7,8 .The least model-dependent search strategies use the production and detection of axions and similar particles by their generic twophoton coupling. It is given by the vertex L aγ = −(1/4) g aγ F µν F µν a = g aγ E · B a, where a is the axion field, F the electromagnetic field-strength tensor, and g aγ a coupling constant of dimension (energy) −1 . Notice that we use natural units with = c = k B = 1. This vertex enables the decay a → γ γ , the Primakoff production in stars-that is, the γ → a scattering in the Coulomb fields of charged particles in the stellar plasma-and the coherent conversion a ↔ γ in laboratory or astrophysical B-fields 9,10 .The helioscope concept, in particular, uses a dipole magnet directed at the Sun to convert axions to...

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“…This process forms the multipolar structure of the magnetic, electric and axion fields around the star. Clearly, every additional n+1 -type moment of the induced field is less by amplitude than the corresponding n-type moment, since every step of this sequential procedure adds the multiplier 1 Ψ0 = g Aγγ , associated with the constant of the axion-photon coupling g Aγγ < 1.47 · 10 −10 Gev −1 [39]. Also, mention should be made that the asymptotic profile of the n+1-type moment differs from the n-type one by the multiplier 1 r , i.e., the n+1-type magnetic, electric and axionic structures are more compact than the n-type ones.…”

Section: Discussionmentioning

confidence: 99%

Magnetoelectrostatics of axionically active systems: Induced field restructuring in magnetic stars

Balakin

Groshev

2020

Phys. Rev. D

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In the framework of Einstein-Maxwell-axion theory we consider a static field configuration in the outer zone of a magnetic star. We assume that this field configuration is formed by the following interacting quartet: a spherically symmetric gravitational field of the Reissner-Nordström type, pseudoscalar field, associated with an axionic dark matter, strong intrinsic magnetic field, and axionically induced electric field. Based on the analysis of the solutions to the master equations of the model, we show that the structure of the formed field configuration reveals the following triple effect. First, if the strong magnetic field of the star has the dipole component, the axionic halo around the magnetic star with spherically symmetric gravitational field is no longer spheroidal, and the distortion is induced by the axion-photon coupling; second, due to the distortion of the axionic halo the magnetic field is no longer pure dipolar, and the induced quadruple, octupole, etc., components appear thus redistributing the magnetic energy between the components with more steep radial profiles than the dipolar one; third, the interaction of the axionic and magnetic fields produces the electric field, which inherits their multipole structure. We attract attention to possible applications of the predicted field restructuring to the theory of axionic rotating magnetars.

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New solar axion search using the CERN Axion Solar Telescope withHe4filling

Cited by 61 publications

References 76 publications

Gaseous time projection chambers for rare event detection: results from the T-REX project. II. Dark matter

Gaseous time projection chambers for rare event detection: results from the T-REX project. II. Dark matter

New CAST limit on the axion–photon interaction

Magnetoelectrostatics of axionically active systems: Induced field restructuring in magnetic stars

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