Pre-inflationary QCD axions form dense stars with densities up to 10^4 eV^4 that contain up to 50% of dark matter after moduli domination.
Detecting Axion Stars with Radio Telescopes
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abstract
When axion stars fly through an astrophysical magnetic background, the axion-to-photon conversion may generate a large electromagnetic radiation power. After including the interference effects of the spacially-extended axion-star source and the macroscopic medium effects, we estimate the radiation power when an axion star meets a neutron star. For a dense axion star with $10^{-13}\,M_\odot$, the radiated power is at the order of $10^{11}\,\mbox{W}\times(100\,\mu\mbox{eV}/m_a)^4\,(B/10^{10}\,\mbox{Gauss})^2$ with $m_a$ as the axion particle mass and $B$ the strength of the neutron star magnetic field. For axion stars occupy a large fraction of dark matter energy density, this encounter event with a transient $\mathcal{O}(0.1\,\mbox{s})$ radio signal may happen in our galaxy with the averaged source distance of one kiloparsec. The predicted spectral flux density is at the order of $\mu$Jy for a neutron star with $B\sim 10^{13}$ Gauss. The existing Arecibo, GBT, JVLA and FAST and the ongoing SKA radio telescopes have excellent discovery potential of dense axion stars.
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Scalar fields in scalar-tensor gravity produce EM radiation through φFμνFμν coupling with resonance amplification that differs from ALP φFμν~Fμν signals, enabling potential distinction and modified gravity tests.
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Pre-inflationary QCD axion stars after moduli domination
Pre-inflationary QCD axions form dense stars with densities up to 10^4 eV^4 that contain up to 50% of dark matter after moduli domination.
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Scalar-Induced Electromagnetic Radiation: Comparison with Axion-Like Particles and Implications for Modified Gravity
Scalar fields in scalar-tensor gravity produce EM radiation through φFμνFμν coupling with resonance amplification that differs from ALP φFμν~Fμν signals, enabling potential distinction and modified gravity tests.