Abstract
We advocate an idea that the presence of the daily and annual modulations of the axion flux on the Earth surface may dramatically change the strategy of the axion searches. Our computations are based on the so-called Axion Quark Nugget (AQN) dark matter model which was originally put forward to explain the similarity of the dark and visible cosmological matter densities $\Omega_{\rm dark}\sim \Omega_{\rm visible}$. In our framework, the population of galactic axions with mass $ 10^{-6} {\rm eV}\lesssim m_a\lesssim 10^{-3}{\rm eV}$ and velocity $< v_a>\sim 10^{-3} c$ will be always accompanied by the axions with typical velocities $<v_a>\sim 0.6 c$ emitted by AQNs. We formulate the broadband detection strategy to search for such relativistic axions by studying the daily and annual modulations. We describe several tests which could effectively discriminate a true signal from noise. These AQN-originated axions can be observed as correlated events which could be recorded by synchronized stations in the global network. The correlations can be effectively studied if the detectors are positioned at distances shorter than a few hundred kilometres.
Highlights
The Peccei-Quinn mechanism, accompanied by axions, remains the most compelling resolution of the strong CP problem, see original papers [1,2,3,4,5,6,7] and recent reviews [8,9,10,11,12,13,14,15,16,17,18]
These axion quark nugget (AQN)-originated axions can be observed as correlated events which could be recorded by synchronized stations in the global network
An important specific feature of the spectrum of the AQN-induced axions that can be used for discriminating against spurious signals is that it has a peak around va ≃ 0.6c with a sharp cutoff at higher velocities around va ≥ 0.8c and a strong suppression at low velocities va ≲ 0.2c, see Fig. 1(a) in [20]
Summary
The Peccei-Quinn mechanism, accompanied by axions, remains the most compelling resolution of the strong CP problem, see original papers [1,2,3,4,5,6,7] and recent reviews [8,9,10,11,12,13,14,15,16,17,18]. This is because they have the same QCD origin and are both proportional to the same fundamental dimensional parameter ΛQCD which ensures that the relation ΩDM ∼ Ωvisible always holds irrespective of the parameters of the model such as the axion mass ma or misalignment angle θ0 The existence of both AQN species explains the observed asymmetry between matter and antimatter as a result of separation of the baryon charge and generation of the disparity between matter and antimatter nuggets as a result of strong CP violation during the QCD epoch. For further details see the original works [40,41,42,43,44,45] with explicit computations of the galactic radiation excesses for various frequencies, including the observed excesses of the diffuse x and γ rays In all these cases the intensity of the photon emission is expressed in terms of a single parameter hBi such that all relative intensities are unambiguously fixed because they are determined by the Standard Model physics. The same comment applies to all other observables such as modulation parameters κðaÞ and κðdÞ and amplification factor AðtÞ to be discussed in the present work
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