Axi-Higgs Cosmology

Fung, Leo WH; Li, Lingfeng; Liu, Tao; Luu, Hoang Nhan; Qiu, Yu-Cheng; Tye, S. -H. Henry

doi:10.48550/arxiv.2102.11257

Cited by 3 publications

(9 citation statements)

References 107 publications

(238 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…(2 meV) 4 where M P 2.4 × 10 18 GeV is the reduced Planck mass, it was realized in Refs. [9,11] that the electroweak (EW) SU (2) instantons with ρ ∼ M −1 P in the minimal supersymmetric extension of the SM (MSSM) can generate the axion potential comparable to the present energy density of DE.…”

Section: Dementioning

confidence: 84%

“…where c is a combination of coefficients of higher dimensional operators used for closing MSSM fermion zero modes emitted from the EW instanton and m SUSY = O(1) TeV is the soft SUSY-breaking mass. 4 In Eq. ( 6), the term 10 compensates the total U (1) F charge of higher dimensional operators closing MSSM fermion zero modes.…”

Section: Dementioning

confidence: 99%

“…cosmic birefringence) may serve as a crucial hint for the presence of new physics beyond the Standard Model (SM), pointing at a source for parity violation in Nature other than weak interactions. When the massive φ is coupled to the SM photon of tensor F µν via an operator ∝ (φ/f φ )F µν F µν , with f φ a decay constant, a nonvanishing ∆φ = φ(t 0 ) − φ(t LSS ) can account for β = 0 [1][2][3][4][5][6] with φ(t 0 ) and φ(t LSS ) evaluated today and at the last scattering surface (LSS) respectively. For reasonable values of the coefficient of the electromagnetic anomaly, β and ∆φ/f φ have similar magnitude.…”

mentioning

confidence: 99%

“…(2 meV) 4 remains unaffected by the change in α 2 (M P ) triggered by introduction of heavy particles charged under SU (2) L [14], the change in RGE of α 2 is expected to cause that of α 1 = g 2 Y /(4π) where g Y is the gauge coupling constant of U (1) Y . The RGE of α 1 is affected by α 2 at the two loop level, so that an increase in α 2 leads to a larger beta function for α 1 .…”

mentioning

confidence: 99%

See 3 more Smart Citations

Cosmic birefringence and electroweak axion dark energy

et al. 2021

View full text Add to dashboard Cite

Taking the recently reported non-zero rotation angle of the cosmic microwave background (CMB) linear polarization β = 0.35±0.14 deg as the hint for a pseudo Nambu-Goldstone boson quintessence dark energy (DE), we study the electroweak (EW) axion quintessence DE model where the axion mass is generated by the EW instantons. We find that the observed value of β implies a non-trivial U (1) electromagnetic anomaly coefficient (cγ), once the current constraint on the DE equation of state is also taken into account. With the aid of the hypothetical high energy structure of the model inspired by the experimentally inferred cγ, the model is shown to be able to make prediction for the current equation of state (wDE,0) of the quintessence DE. This is expected to make our scenario distinguishable in comparison with the cosmological constant (w = −1) and testable in future when the error in the future measurement of wDE,0 is reduced to O(1)% level (δw = O(10 −2 )).

show abstract

Section: Dementioning

confidence: 84%

Section: Dementioning

confidence: 99%

mentioning

confidence: 99%

mentioning

confidence: 99%

See 2 more Smart Citations

Cosmic birefringence and electroweak axion dark energy

et al. 2021

View full text Add to dashboard Cite

show abstract

“…The authors of Ref. [947] present a simple model in which a light axion is coupled to the Higgs field. In this scenario, the Higgs vacuum expectation value in the early Universe is larger than its measured value, thus modifying the electron rest mass and possibly alleviating the Hubble tension (see Section 12.1).…”

Section: Axi-higgs Modelmentioning

confidence: 99%

In the Realm of the Hubble tension $-$ a Review of Solutions

Di Valentino,

Mena,

Pan

et al. 2021

Preprint

178

252

View full text Add to dashboard Cite

The simplest ΛCDM model provides a good fit to a large span of cosmological data but harbors large areas of phenomenology and ignorance. With the improvement of the number and the accuracy of observations, discrepancies among key cosmological parameters of the model have emerged. The most statistically significant tension is the 4σ to 6σ disagreement between predictions of the Hubble constant, H 0 , made by the early time probes in concert with the "vanilla" ΛCDM Cosmological model, and a number of late time, model-independent determinations of H 0 from local measurements of distances and redshifts. The high precision and consistency of the data at both ends present strong challenges to the possible solution space and demands a hypothesis with enough rigor to explain multiple observations-whether these invoke new physics, unexpected large-scale structures or multiple, unrelated errors. A thorough review of the problem including a discussion of recent Hubble constant estimates and a summary of the proposed theoretical solutions is presented here. We include more than 850 references, indicating that the interest in this area has grown considerably just during the last few years. We classify the many proposals to resolve the tension in these categories: Early Dark Energy, Late Dark Energy, Dark energy models with 6 degrees of freedom and their extensions, Models with extra relativistic degrees of freedom, Models with Extra Interactions, Unified cosmologies, Modified gravity, Inflationary models, Modified recombination history, Physics of the critical Phenomena, and Alternative proposals. Some are formally successful, improving the fit to the data in light of their additional degrees of freedom, restoring agreement within 1 − 2σ between Planck 2018, using the Cosmic Microwave Background power spectra data, Baryon Acoustic Oscillations, Pantheon SN data, and R20, the latest SH0ES Team [2] measurement of the Hubble constant (H 0 = 73.2 ± 1.3 km s −1 Mpc −1 at 68% confidence level). However, there are many more unsuccessful models which leave the discrepancy well above the 3σ disagreement level. In many cases, reduced tension comes not simply from a change in the value of H 0 but also due to an increase in its uncertainty due to degeneracy with additional physics, complicating the picture and pointing to the need for additional probes. While no specific proposal makes a strong case for being highly likely or far better than all others, solutions involving early or dynamical dark energy, neutrino interactions, interacting cosmologies, primordial magnetic fields, and modified gravity provide the best options until a better alternative comes along.

show abstract

In the realm of the Hubble tension—a review of solutions ^*

Valentino

Mena²,

Pan³

et al. 2021

Class. Quantum Grav.

1,302

760

View full text Add to dashboard Cite

The simplest ΛCDM model provides a good fit to a large span of cosmological data but harbors large areas of phenomenology and ignorance. With the improvement of the number and the accuracy of observations, discrepancies among key cosmological parameters of the model have emerged. The most statistically significant tension is the 4σ to 6σ disagreement between predictions of the Hubble constant, H 0, made by the early time probes in concert with the ‘vanilla’ ΛCDM cosmological model, and a number of late time, model-independent determinations of H 0 from local measurements of distances and redshifts. The high precision and consistency of the data at both ends present strong challenges to the possible solution space and demands a hypothesis with enough rigor to explain multiple observations—whether these invoke new physics, unexpected large-scale structures or multiple, unrelated errors. A thorough review of the problem including a discussion of recent Hubble constant estimates and a summary of the proposed theoretical solutions is presented here. We include more than 1000 references, indicating that the interest in this area has grown considerably just during the last few years. We classify the many proposals to resolve the tension in these categories: early dark energy, late dark energy, dark energy models with 6 degrees of freedom and their extensions, models with extra relativistic degrees of freedom, models with extra interactions, unified cosmologies, modified gravity, inflationary models, modified recombination history, physics of the critical phenomena, and alternative proposals. Some are formally successful, improving the fit to the data in light of their additional degrees of freedom, restoring agreement within 1–2σ between Planck 2018, using the cosmic microwave background power spectra data, baryon acoustic oscillations, Pantheon SN data, and R20, the latest SH0ES Team Riess, et al (2021 Astrophys. J. 908 L6) measurement of the Hubble constant (H 0 = 73.2 ± 1.3 km s−1 Mpc−1 at 68% confidence level). However, there are many more unsuccessful models which leave the discrepancy well above the 3σ disagreement level. In many cases, reduced tension comes not simply from a change in the value of H 0 but also due to an increase in its uncertainty due to degeneracy with additional physics, complicating the picture and pointing to the need for additional probes. While no specific proposal makes a strong case for being highly likely or far better than all others, solutions involving early or dynamical dark energy, neutrino interactions, interacting cosmologies, primordial magnetic fields, and modified gravity provide the best options until a better alternative comes along.

show abstract

Axi-Higgs Cosmology

Cited by 3 publications

References 107 publications

Cosmic birefringence and electroweak axion dark energy

Cosmic birefringence and electroweak axion dark energy

In the Realm of the Hubble tension $-$ a Review of Solutions

In the realm of the Hubble tension—a review of solutions ^*

Contact Info

Product

Resources

About

Axi-Higgs Cosmology

Cited by 3 publications

References 107 publications

Cosmic birefringence and electroweak axion dark energy

Cosmic birefringence and electroweak axion dark energy

In the Realm of the Hubble tension $-$ a Review of Solutions

In the realm of the Hubble tension—a review of solutions *

Contact Info

Product

Resources

About

In the realm of the Hubble tension—a review of solutions ^*