学术文献库

Dark compact objects ("clumps") transiting the Solar System exert accelerations on the test masses (TM) in a gravitational-wave (GW) detector. We reexamine the detectability of these clump transits in a variety of current and future GW detectors, operating over a broad range of frequencies. TM accelerations induced by clump transits through the inner Solar System have frequency content around $f \sim μ$Hz. Some of us [arXiv:2112.11431] recently proposed a GW detection concept with $μ$Hz sensitivity, based on asteroid-to-asteroid ranging. From the detailed sensitivity projection for this concept, we find both analytically and in simulation that purely gravitational clump-matter interactions would yield one detectable transit every $\sim 20$ yrs, if clumps with mass $m_{\text{cl}} \sim 10^{14} \text{kg}$ saturate the dark-matter (DM) density. Other (proposed) GW detectors using local TMs and operating in higher frequency bands are sensitive to smaller clump masses and have smaller rates of discoverable signals. We also consider the case of clumps endowed with an additional attractive long-range clump-matter fifth force significantly stronger than gravity (but evading known fifth-force constraints). For the $μ$Hz detector concept, we use simulations to show that, for example, a clump-matter fifth-force $\sim 10^3$ times stronger than gravity with a range of $\sim\text{AU}$ would boost the rate of detectable transits to a few per year for clumps in the mass range $10^{11} \text{kg} \lesssim m_{\text{cl}} \lesssim 10^{14} \text{kg}$, even if they are a $\sim 1$% sub-component of the DM. The ability of $μ$Hz GW detectors to probe asteroid-mass-scale dark objects that may otherwise be undetectable bolsters the science case for their development.