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P Log-Uniform P1 2 ms P2 15 ms ρ2 χ2 k 2 σρ 5 kpc z Exponential z0 1 kpc B Log-Normal µB 12.5 [log10 G] σB 0.7 [log10 G] TABLE I

We also make a constantBassumption in our models, ignoring Ohmic dissipation, other magnetic field weakening mechanisms, as well as any spin-up processes that would produce millisecond pulsars · 2018

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Detecting the Axion-Photon Conversion Background

astro-ph.HE · 2026-05-14 · unverdicted · novelty 5.0

Neutron star magnetospheres across the Milky Way produce a faint but statistically detectable axion-photon conversion radio background, while interstellar medium signals are too weak for current instruments.

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  • Detecting the Axion-Photon Conversion Background astro-ph.HE · 2026-05-14 · unverdicted · none · ref 1

    Neutron star magnetospheres across the Milky Way produce a faint but statistically detectable axion-photon conversion radio background, while interstellar medium signals are too weak for current instruments.