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Title: Opening up the QCD axion window

Abstract

We present a new mechanism to deplete the energy density of the QCD axion, making decay constants as high as f a ≃ 10 17 GeV viable for generic initial conditions. In our setup, the axion couples to a massless dark photon with a coupling that is moderately stronger than the axion coupling to gluons. Dark photons are produced copiously through a tachyonic instability when the axion field starts oscillating, and an exponential suppression of the axion density can be achieved. For a large part of the parameter space this dark radiation component of the universe can be observable in upcoming CMB experiments. Such dynamical depletion of the axion density ameliorates the isocurvature bound on the scale of inflation. The depletion also amplifies the power spectrum at scales that enter the horizon before particle production begins, potentially leading to axion miniclusters.

Authors:
 [1];  [2];  [3]
  1. Harvard Univ., Cambridge, MA (United States). Dept. of Physics
  2. Stanford Univ., CA (United States). Stanford Institute for Theoretical Physics
  3. Massachusetts Inst. of Technology (MIT), Cambridge, MA (United States). Center for Theoretical Physics
Publication Date:
Research Org.:
Stanford Univ., CA (United States); Massachusetts Inst. of Tech., Cambridge, MA (United States)
Sponsoring Org.:
USDOE Office of Science (SC)
OSTI Identifier:
1499139
Grant/Contract Number:  
SC0012012; SC0012567; SC0015476
Resource Type:
Accepted Manuscript
Journal Name:
Journal of High Energy Physics (Online)
Additional Journal Information:
Journal Name: Journal of High Energy Physics (Online); Journal Volume: 2018; Journal Issue: 3; Journal ID: ISSN 1029-8479
Publisher:
Springer Berlin
Country of Publication:
United States
Language:
English
Subject:
72 PHYSICS OF ELEMENTARY PARTICLES AND FIELDS

Citation Formats

Agrawal, Prateek, Marques-Tavares, Gustavo, and Xue, Wei. Opening up the QCD axion window. United States: N. p., 2018. Web. doi:10.1007/jhep03(2018)049.
Agrawal, Prateek, Marques-Tavares, Gustavo, & Xue, Wei. Opening up the QCD axion window. United States. doi:10.1007/jhep03(2018)049.
Agrawal, Prateek, Marques-Tavares, Gustavo, and Xue, Wei. Thu . "Opening up the QCD axion window". United States. doi:10.1007/jhep03(2018)049. https://www.osti.gov/servlets/purl/1499139.
@article{osti_1499139,
title = {Opening up the QCD axion window},
author = {Agrawal, Prateek and Marques-Tavares, Gustavo and Xue, Wei},
abstractNote = {We present a new mechanism to deplete the energy density of the QCD axion, making decay constants as high as fa ≃ 1017 GeV viable for generic initial conditions. In our setup, the axion couples to a massless dark photon with a coupling that is moderately stronger than the axion coupling to gluons. Dark photons are produced copiously through a tachyonic instability when the axion field starts oscillating, and an exponential suppression of the axion density can be achieved. For a large part of the parameter space this dark radiation component of the universe can be observable in upcoming CMB experiments. Such dynamical depletion of the axion density ameliorates the isocurvature bound on the scale of inflation. The depletion also amplifies the power spectrum at scales that enter the horizon before particle production begins, potentially leading to axion miniclusters.},
doi = {10.1007/jhep03(2018)049},
journal = {Journal of High Energy Physics (Online)},
number = 3,
volume = 2018,
place = {United States},
year = {2018},
month = {3}
}

Journal Article:
Free Publicly Available Full Text
Publisher's Version of Record

Citation Metrics:
Cited by: 21 works
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Figures / Tables:

Figure 1 Figure 1: Current bounds and future experimental reach for axion couplings to photons de ned in eq. (2.1). Blue shaded regions show the current constraints which are independent of a dark matter interpretation, while the red shaded region are constraints from axion haloscopes. Sensitivity of future experiments is shown bymore » colored lines. The thick black line shows the prediction for the KSVZ axion as in eq. (2.2). The solid part of the line indicates where the initial misalignment would need to be tuned θi < 0.1 or worse, which is where our mechanism is needed to have the correct axion abundance. For larger values of fa (the green part of the line) the extra dark radiation produced by our mechanism will be within the sensitivity of future CMB experiments. Even larger fa values (the gray part), are already constrained by Planck observations (see discussion in section 4.3).« less

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    Figures/Tables have been extracted from DOE-funded journal article accepted manuscripts.