The QCD axion, precisely

By G. G. Cortona, Edward Hardy, Javier Pardo Vega, G. Villadoro. 2015

658 citations recorded by the source corpus.

A bstractWe show how several properties of the QCD axion can be extracted at high precision using only first principle QCD computations. By combining NLO results obtained in chiral perturbation theory with recent Lattice QCD results the full axion potential, its mass and the coupling to photons can be reconstructed with percent precision. Axion couplings to nucleons can also be derived reliably, with uncertainties smaller than ten percent. The approach presented here allows the precision to be further improved as uncertainties on the light quark masses and the effective theory couplings are reduced. We also compute the finite temperature dependence of the axion potential and its mass up to the crossover region. For higher temperature we point out the unreliability of the conventional instanton approach and study its impact on the computation of the axion relic abundance.

Subfields: Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/722f9cf7025f366ead338a835f8cf1e3d41ce7e5

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In Nuclear and High Energy Physics

Citations in the corpus

Stellar recipes for axion hunters (2017, methodology): “as found in the state-of-the-art calculation [40].”
A Review of Gravitational Waves from Cosmic Domain Walls (2017, background): “The global U(1) PQ symmetry is explicitly broken to its subgroup ZN due to topological charge fluctuations in the QCD vacuum [82,83], and the effective potential for the axion field a at low energies is described by that in Equation (7), where the axion mass is given by m ∼ Fπmπ/F ∼ 6 μeV (1012 GeV/”
Using the Full Power of the Cosmic Microwave Background to Probe Axion Dark Matter (2017, background): “Axions which obtain their mass from a gauge theory Chern-Simons interaction have a temperature (and thus time) dependent mass, and a calculable self-interaction potential (e.g. di Cortona et al. 2016; Davoudiasl & Murphy 2017).”
Recent Progress in the Physics of Axions and Axion-Like Particles (2020, background): “Here we use the result of [57] for gaN (N = p, n), σπN = 1 2(mu + md)〈N |(ūu + d̄d)|N〉 ' 42 MeV for ḡaN [58], and ignore the contribution to ḡaγ from θQCD.”
The landscape of QCD axion models (2020, methodology): “undaryA0 = ig 1 s U 1@ U. Conﬁgurationsofthistypeare 4Weadoptthefollowingconventions: D = @ igsTaAa ,Ga = @Aa Aa+ gsfabcAaAaandG~a = 1 2 ˆ˙Gaˆ˙ with0123 = 1. Thelatterconventionisusedin[47],whileforinstanceRef.[39]employs0123 = +1. 7 calledapure gauges. Weareinterestedinpuregaugesforwhich Ucannotbe”
The photo-philic QCD axion (2016, background): “re present at low energy even if they are absent in the UV, while this is not true for the electron coupling. The axion has its minimum for hai= f a QCD and V(a) is a cosine function, approximately [17]. The very small axion mass in Eq. (4) makes the axion a viable DM candidate. As the universe cool”
New experimental approaches in the search for axion-like particles (2018, methodology): “(7)Our conventions are essentially the same as [67] so we can directly take their results.”
More axions from strings (2020, background): “his 11The temperature dependence and the form of the axion potential is expected to change at T˘ c’155 MeV and below, where the axion potential is well approximated by the zero temperature prediction [43]. However, we will see that for the range of parameters relevant for the QCD axion dark matter, ”
Early seeds of axion miniclusters (2018, background): “cently, ˜T(T) has been calculated in lattice QCD up to T˘2 GeV [16]. The axion mass increases very abruptly as the universe’s temperature decreases and saturates at a value ˜0 = (75:5(5)MeV)4 below Tc[15,16], which allows to dene the zero-Taxion mass, mA(T= 0) = p ˜0 fA = 57 eV 1011GeV fa : (2.3) ”
Improved axion emissivity from a supernova via nucleon-nucleon bremsstrahlung (2019, background): “ C ai; (2.3) where f a is the Peccei-Quinn energy scale and m N is the nucleon mass (we assume m n ’ m p). The coupling constants, C ai, for the benchmark axion models have been recently calculated [5]. Their most accurate values, including the uncertainties, are CKSVZ ap = 0:47(3); CKSVZ an = 0:02”