QCD axion as a bridge between string theory and flavor physics

Ahn, Y. H.

doi:10.1103/physrevd.93.085026

Cited by 9 publications

(18 citation statements)

References 42 publications

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“…Here we discuss that the global U(1) X is the remnant of the broken U(1) X gauge symmetry by the GS mechanism, and so it can be protected from quantum-gravitational effects, similar to Ref. [2]. String theory when compactified to four dimensions generically contains an anomalous U(1) with anomaly cancellation.…”

Section: B Quarks Leptons and Axionsmentioning

confidence: 73%

“…Below the scale where the complex structure and the axio-dilaton moduli are stabilized through fluxes as in Refs. [41,42], the low-energy Kahler potential K and superpotential W for the Kahler moduli and matter superfields, invariant under U(1) X gauged symmetry, are given in type IIB string theory by [2]…”

Section: B Quarks Leptons and Axionsmentioning

confidence: 99%

“…Here the global U (1) X symmetry is a remnant of the broken U (1) X gauge symmetry which connects string theory with flavor physics [2], see Sec. II C. basis vectors for two 3's.…”

Section: Introductionmentioning

confidence: 99%

“…It indicates that the gravitino mass (or soft SUSY breaking mass, m S = m 3/2 , see Ref. [2]) strongly depends on the scales of PQ fields and Φ T as well as the ratios √ α 1 α 2 /|α| 2 and β 1 /γ(β + γ); for example, for…”

Section: Introductionmentioning

confidence: 99%

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Axion and neutrino physics in aU(1)-enhanced supersymmetric model

Ahn

2017

Phys. Rev. D

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Motivated by the flavored Peccei-Quinn symmetry for unifying the flavor physics and string theory, we construct an explicit model by introducing a U (1) symmetry such that the U (1) X -[gravity] 2 anomaly-free condition together with the standard model flavor structure demands additional sterile neutrinos as well as no axionic domain-wall problem. Such additional sterile neutrinos play the role of a realization of baryogenesis via a new Affleck-Dine leptogenesis. We provide grounds for that the U (1) X symmetry could be interpreted as a fundamental symmetry of nature. The model will resolve rather recent, but fast-growing issues in astro-particle physics, including leptonic mixings and CP violation in neutrino oscillation, high-energy neutrinos, QCD axion, and axion cooling of stars. The QCD axion decay constant, through its connection to the astrophysical constraints of stellar evolution and the SM fermion masses, is shown to be fixed at F A = 1.30 +0.66 −0.54 ×10 9 GeV (consequently, its mass is m a = 4.34 +3.37 −1.49 meV and axion-photon coupling is |g aγγ | = 1.30 +1.01 −0.45 ×10 −12 GeV −1 ). Interestingly enough, we show that neutrino oscillations at low energies could be connected to astronomical-scale baseline neutrino oscillations. The model predicts non-observational neutrinoless double beta (0νββ) decay rate as well as a remarkable pattern between leptonic Dirac CP phase (δ CP ) and atmospheric mixing angle (θ 23 ); e.g. δ CP ≃ 220 • −240 • , 120 • −140 • for θ 23 = 42.3 • for normal mass ordering, and δ CP ≃ 283 • , 250 • , 100 • , 70 • for θ 23 = 49.5 • for inverted one. We stress that future measurements on θ 23 , 0νββ decay rate, sum of active neutrino masses, track-to-shower ratio of a cosmic neutrino, astrophysical constraints on axions, QCD axion mass, and its axion-photon coupling are of importance to test the model in the near future. * Electronic address: yhahn@ibs.re.kr may be hidden from our sight at all wavelengths of the electromagnetic spectrum because of absorption by matter and radiation between us and the source. So, data from a variety of observational windows, especially, through direct observations with neutrinos and axions, may be crucial. Thus, the axions and neutrinos in astrophysics and cosmology could provide a natural laboratory for a new extension of SM particle physics 3 .Axions in stars available at low energies are well suited for very sensitive tests. If the axion exists, it solves the strong CP problem of QCD through the Peccei-Quinn (PQ) mechanism [5,6], fits easily into a string theoretic framework, and appears cosmologically as a form of cold dark matter. The axion lies at the intersection of elementary particle physics, astrophysics, cosmology and string theory, potentially playing a crucial role in each. There are being 1 In Ref. [2] a concrete model is designed to bridge between string theory as a fundamental theory and low energy flavor physics. 2 Ref. [1] introduces a superpotential for unifying flavor and strong CP problems, the so-called flavored PQ symmetry m...

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Section: B Quarks Leptons and Axionsmentioning

confidence: 73%

Section: B Quarks Leptons and Axionsmentioning

confidence: 99%

“…Here the global U (1) X symmetry is a remnant of the broken U (1) X gauge symmetry which connects string theory with flavor physics [2], see Sec. II C. basis vectors for two 3's.…”

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Axion and neutrino physics in aU(1)-enhanced supersymmetric model

Ahn

2017

Phys. Rev. D

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“…Motivated by the flavored PQ symmetry for unifying the flavor physics and string theory [1,7], we have constructed a compact model based on SL 2 (F 3 ) × U(1) X symmetry for resolving rather recent, but fast-growing issues in astro-particle physics, including quark and leptonic mixings and CP violations, high-energy neutrinos, QCD axion, and axion cooling of stars. Since astro-particle physics observations have increasingly placed tight constraints on parameters for flavored-axions, we have showed how the scale responsible for PQ mechanism (congruent to that of seesaw mechanism) could be fixed, and in turn the scale responsible for FN mechanism through flavor physics.…”

Section: Discussionmentioning

confidence: 99%

Compact model for quarks and leptons via flavored axions

Ahn

2018

Phys. Rev. D

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We show how the scales responsible for Peccei-Quinn (PQ), seesaw, and Froggatt and Nielsen (FN) mechanisms can be fixed, by constructing a compact model for resolving rather recent, but fast-growing issues in astro-particle physics, including quark and leptonic mixings and CP violations, high-energy neutrinos, QCD axion, and axion cooling of stars. The model is motivated by the flavored PQ symmetry for unifying the flavor physics and string theory. The QCD axion decay constant congruent to the seesaw scale, through its connection to the astro-particle constraints of both the stellar evolution induced by the flavored-axion bremsstrahlung off electrons e + Ze → Ze + e + A i and the rare flavor-changing decay process induced by the flavored-axion−0.84 × 10 10 GeV (consequently, the QCD axion mass m a = 1.54 +0.48 −0.29 × 10 −4 eV, Compton wavelength of its oscillation λ a = 8.04 +1.90 −1.90 mm, and axion to neutron coupling g Ann = 2.14 +0.66 −0.41 × 10 −12 , etc.). Subsequently, the scale associated to FN mechanism is dynamically fixed, Λ = 2.04 +0.48 −0.48 × 10 11 GeV, through its connection to the standard model fermion masses and mixings, and such fundamental scale might give a hint where some string moduli are stabilized in type-IIB string vacua. In the near future, the NA62 experiment expected to reach the sensitivity of Br(K + → π + + A i ) < 1.0 × 10 −12 will probe the flavored-axions or exclude the model, if the astrophysical constraint of star cooling is really responsible for the flavored-axion. PACS numbers: * Here 'compact' model means a model that provides only requisite parameters it is easy to disprove. † Electronic address: axionahn@naver.com 1 See, most recent its related simple toy models ((non-)supersymmetric versions) in Ref . [5], see also Ref. [6]. 2 On this issue we will consider flavored-axion [8] as a cold dark matter in the next project. The scale in Eq. (44) we found is available for explaining dark matter, and finding it in experiments can change the fundamental understanding of the universe.

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One‐parametric description for scalar field dark matter potentials

Cedeño

Ureña–López

2021

Astron Nachr

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We study the cosmological evolution for a scalar field dark matter model, by considering a parameterization of the evolution equations that allow us to unify in a single parameter a family of potentials: quadratic (free case), trigonometric (Axionlike case), and hyperbolic. After exploring the cosmological dynamics of this model, we perform a statistical analysis to study the viability of such model in comparison with the standard Cold Dark Matter model. We found that the free case is preferred over the other scalar field potentials, but in any case all of them are disfavored by the cosmological observations with respect to the standard model.

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QCD axion as a bridge between string theory and flavor physics

Cited by 9 publications

References 42 publications

Axion and neutrino physics in aU(1)-enhanced supersymmetric model

Axion and neutrino physics in aU(1)-enhanced supersymmetric model

Compact model for quarks and leptons via flavored axions

One‐parametric description for scalar field dark matter potentials

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