Тёмная материя вокруг чёрных дыр: как услышать невидимое экспресс

Оригинальная аннотация

как её написали авторы, на английском arXiv:2605.17589

Ultralight bosons with self-interactions, such as axion-like particles, can form astrophysical Bose--Einstein condensates around stars or compact objects, often referred to as gravitational atoms. In this work, we adopt a recently proposed dynamical formation mechanism for these halos and estimate their impact on extreme- and intermediate-mass-ratio inspirals when present around the primary black hole. We show that, for signal-to-noise ratios $$\lesssim 100$$, LISA can distinguish gravitational waveforms from binaries embedded in such halo overdensities. Our analysis indicates that LISA can probe boson masses $$m_\mathrm{dm}\sim10^{-17}$$--$$10^{-15}\,\mathrm{eV}$$ and decay constants $$f_a\sim3 \times 10^{10}$$--$$6 \times 10^{12}\,\mathrm{GeV}$$ using binaries with total masses $$M\sim10^4$$--$$10^5\,M_\odot$$, assuming conservative DM densities consistent with the central values of Navarro--Frenk--White profiles. Allowing for higher background densities and different extreme-mass-ratio configurations further extends the accessible parameter space. Moreover, we find that for a binary configuration with $$M\sim10^4M_{\odot}$$, $$\rho_{\rm dm} = 10^4\,\mathrm{GeV/cm^3}$$, and signal to noise ratio $$\text{SNR} \sim 20$$, a particle mass of $$m_{dm} = 3.2 \cdot 10^{-15}$$ eV and decay constant of $$f_a = 1.6 \cdot 10^{11}$$ GeV maximize the dephasing due to dynamical friction, enabling the recovery of the particle parameters at the percent level. These results demonstrate that LISA can place constraints on axion-like particle masses and self-interactions without requiring additional couplings to Standard Model fields.