Лазерный детектор услышит шёпот тёмной материи экспресс

Оригинальная аннотация

как её написали авторы, на английском arXiv:2606.16099

A coherent cosmic background of axion-like particles (ALPs) coupled to photons can produce a small periodic differential phase or polarization modulation for photons traversing separate arms in gravitational wave interferometers, peaked at a frequency associated with the particle mass, and suppressed whenever the dark-matter coherence length $$\lambda_{\rm coh}$$ exceeds the arm length~$$L$$. For the LIGO audio frequency band the sensitivity to cosmic ALPs is below current bounds. For LISA, however, the natural mass range $$m_a \sim 4\times10^{-19}$$--$$4\times10^{-16}$$~eV -- corresponding to a sideband frequency in LISA's science band of $$0.1$$~mHz--$$0.1$$~Hz -- may be observable. A 1-year shot-noise-limited search projects a sensitivity $$g_{a\gamma\gamma} \lesssim 5\times 10^{-14}$$~GeV$$^{-1}$$ across most of the band, reaching $$\sim 7\times 10^{-15}$$~GeV$$^{-1}$$ near $$0.1$$~Hz, which is $$10^{3}$$--$$10^{4}$$ below the CAST helioscope bound. An RF heterodyne photodetection upgrade -- to either detector -- might extend the search sensitivity to $$g_{a\gamma\gamma}\sim 6.5\times 10^{-14}$$~GeV$$^{-1}$$ at $$m_a\sim 3\times 10^{-7}$$~eV for LIGO and $$g_{a\gamma\gamma}\sim 3.3\times 10^{-17}$$~GeV$$^{-1}$$ at $$m_a\sim 5\times 10^{-13}$$~eV for LISA. Dark-matter substructure can affect the signal in a several interesting ways.