Axion Condensate Dark Matter Constraints from Resonant Enhancement of Background Radiation

Sigl, G.; Trivedi, Pranjal

doi:10.48550/arxiv.1907.04849

Cited by 14 publications

(19 citation statements)

References 45 publications

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“…The lifetimes of inflaton clusters and stars depend on their couplings to other particles. Interestingly, inflaton stars locally restore the coherence of the inflaton field and can therefore decay by parametric resonance, analogously to the resonant decay of axion stars into photons [14,28,29].…”

Section: Conclusion and Discussionmentioning

confidence: 99%

Inflaton Clusters and Inflaton Stars

Niemeyer,

Easther

2019

Preprint

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In a broad class of scenarios, inflation is followed by an extended era of matter-dominated expansion during which the inflaton condensate is nonrelativistic on subhorizon scales. During this phase density perturbations grow to the point of nonlinearity and collapse into bound structures. This epoch strongly resembles structure formation with ultra-light axion-like particles. This parallel permits us to adapt results from studies of cosmological structure formation to describe the nonlinear dynamics of this post-inflationary epoch. We show that the inflaton condensate fragments into "inflaton clusters", analogues of axion dark matter halos in present-day cosmology. Moreover, solitonic objects or "inflaton stars" can form inside these clusters, leading to density contrasts as large as 10 6 in the post-inflationary universe.

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Section: Conclusion and Discussionmentioning

confidence: 99%

Inflaton Clusters and Inflaton Stars

Niemeyer,

Easther

2019

Preprint

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“…A common strategy is to exploit a putative axion-photon coupling. This coupling could be detected through the decay of axions to photons (which can be stimulated [225][226][227][228][229][230][231][232] or resonantly enhanced [233][234][235][236][237][238][239][240][241]), axion-photon mixing in an external magnetic field [242] (which can notably also imprint an asymmetry on the polarization spectrum, see [e.g. 243]), birefringence [244][245][246][247][248][249][250][251], or the production of axions from non-orthogonal electric and magnetic fields [252].…”

Section: Axion Indirect Detectionmentioning

confidence: 99%

Astrophysical and Cosmological Probes of Dark Matter

Boddy¹,

Lisanti²,

McDermott³

et al. 2022

Preprint

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While astrophysical and cosmological probes provide a remarkably precise and consistent picture of the quantity and general properties of dark matter, its fundamental nature remains one of the most significant open questions in physics. Obtaining a more comprehensive understanding of dark matter within the next decade will require overcoming a number of theoretical challenges: the groundwork for these strides is being laid now, yet much remains to be done. Chief among the upcoming challenges is establishing the theoretical foundation needed to harness the full potential of new observables in the astrophysical and cosmological domains, spanning the early Universe to the inner portions of galaxies and the stars therein. Identifying the nature of dark matter will also entail repurposing and implementing a wide range of theoretical techniques from outside the typical toolkit of astrophysics, ranging from effective field theory to the dramatically evolving world of machine learning and artificial-intelligence-based statistical inference. Through this work, the theory frontier will be at the heart of dark matter discoveries in the upcoming decade.

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“…While originally motivated as a solution to the strong CP problem [18][19][20], they are ubiquitous in many high energy physics theories [21][22][23][24]. A variety of experimental efforts are underway to detect axions and axion-like particles (ALPs) in the laboratory [25][26][27][28] and through their unique astrophysical and cosmological signatures [29][30][31][32][33][34][35][36][37][38]. Many of these searches rely upon a coupling of the axion field φ(x, t) to electromagnetism via the interaction g aγ φE • B.…”

Section: Introductionmentioning

confidence: 99%

Dipole Radiation and Beyond from Axion Stars in Electromagnetic Fields

Amin,

Long,

Mou

et al. 2021

Preprint

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We investigate the production of photons from coherently oscillating, spatially localized clumps of axionic fields (oscillons and axion stars) in the presence of external electromagnetic fields. We delineate different qualitative behaviour of the photon luminosity in terms of an effective dimensionless coupling parameter constructed out of the axion-photon coupling, and field amplitude, oscillation frequency and radius of the axion star. For small values of this dimensionless coupling, we provide a general analytic formula for the dipole radiation field and the photon luminosity per solid angle, including a strong dependence on the radius of the configuration. For moderate to large coupling, we report on a non-monotonic behavior of the luminosity with the coupling strength in the presence of external magnetic fields. After an initial rise in luminosity with the coupling strength, we see a suppression (by an order of magnitude or more compared to the dipole radiation approximation) at moderately large coupling. At sufficiently large coupling, we find a transition to a regime of exponential growth of the luminosity due to parametric resonance. We carry out 3+1 dimensional lattice simulations of axion electrodynamics, at small and large coupling, including non-perturbative effects of parametric resonance as well as backreaction effects when necessary. We also discuss medium (plasma) effects that lead to resonant axion to photon conversion, relevance of the coherence of the soliton, and implications of our results in astrophysical and cosmological settings.

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Axion Condensate Dark Matter Constraints from Resonant Enhancement of Background Radiation

Cited by 14 publications

References 45 publications

Inflaton Clusters and Inflaton Stars

Inflaton Clusters and Inflaton Stars

Astrophysical and Cosmological Probes of Dark Matter

Dipole Radiation and Beyond from Axion Stars in Electromagnetic Fields

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