Dark matter axions revisited

By Luca Visinelli, P. Gondolo. 2009

215 citations recorded by the source corpus.

We study for what specific values of the theoretical parameters the axion can form the totality of cold dark matter. We examine the allowed axion parameter region in the light of recent data collected by the WMAP5 mission plus baryon acoustic oscillations and supernovae, and assume an inflationary scenario and standard cosmology. We also upgrade the treatment of anharmonicities in the axion potential, which we find important in certain cases. If the Peccei-Quinn symmetry is restored after inflation, we recover the usual relation between axion mass and density, so that an axion mass m{sub a}=(85{+-}3) {mu}eV makes the axion 100% of the cold dark matter. If the Peccei-Quinn symmetry is broken during inflation, the axion can instead be 100% of the cold dark matter for m{sub a}<15 meV provided a specific value of the initial misalignment angle {theta}{sub i} is chosen in correspondence to a given value of its mass m{sub a}. Large values of the Peccei-Quinn symmetry breaking scale correspond to small, perhaps uncomfortably small, values of the initial misalignment angle {theta}{sub i}.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/c5b25d19cf043050666a9bfefb5d77d92a29bb39

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Citations in the corpus

Dark matter direct-detection experiments (2015, background): “parameters, axions could account for the complete missing matter [64].”
TASI Lectures on the Strong CP Problem and Axions (2018, unknown): “The simplest way is to tune θ ∼ π [123, 124, 125].”
Euclidean Wormholes, Baby Universes, and Their Impact on Particle Physics and Cosmology (2018, methodology): “Using the approximate analytic expression for f(θi) given in [160], one can estimate that an initial tuning θi ≈ 0.”
Cosmology and Fundamental Physics with the Euclid Satellite (2012, background): “They are similar to the well known QCD axion (Peccei and Quinn 1977; Weinberg 1978; Wilczek 1978; ’t Hooft 1976b, a; Dine 1981; Preskill et al. 1983; Steinhardt and Turner 1983; Turner et al. 1983; Abbott and Sikivie 1983; Dine and Fischler 1983; Turner 1986; Visinelli and Gondolo 2009), and their c”
The landscape of QCD axion models (2020, background): “The change in the slope corresponds to the effect of the non-harmonic terms in the axion potential when θi & O(1) [173].”
Physics reach of the XENON1T dark matter experiment. (2015, unknown): “exist, like axions [10], superheavy particles [11] and sterile neutrinos [12], in this study we will focus on the detection of WIMPs.”
The dark-matter axion mass (2017, background): “PQ symmetry is restored either during or at some point after inflation, so that the axion field starts out “random,” meaning that its value at points out of post-inflationary causal contact are uncorrelated [14, 15];”
Axion cosmology revisited (2009, methodology): “This is in agreement with the earlier numerical work by [76] and analytic computations [56, 74, 80].”