McQuinn, MatthewMcGrath, Casey2025-01-082025-01-082024-11-22https://doi.org/10.48550/arXiv.2411.15072http://hdl.handle.net/11603/37136The microhertz frequency band of gravitational waves probes the merger of supermassive black holes as well as many other gravitational wave phenomena. However, space-interferometry methods that use test masses would require substantial development of test-mass isolation systems to detect anticipated astrophysical events. We propose an approach that avoids inertial test masses by situating spacecraft in the low-acceleration environment of the outer Solar System. We show that for Earth-spacecraft and inter-spacecraft distances of ≳10 AU, the accelerations on the spacecraft would be sufficiently small to potentially achieve sensitivities determined by stochastic gravitational wave backgrounds. We further argue, for arm lengths of 10−30 AU and 10 Watt transmissions, that stable phase locks should be achievable with 20 cm mirrors or 5 m radio dishes. We discuss designs that send both laser beams and radio waves between the spacecraft, finding that despite the ∼10 ⁴× longer wavelengths, even a design with radio transmissions could reach stochastic background-limited sensitivities at ≲0.3×10⁻⁴ Hz. Operating in the radio significantly reduces many spacecraft design tolerances. Our baseline concept requires two arms to do interferometry. However, if one spacecraft carries a clock with Allan deviations at 10 ⁴ seconds of 10⁻¹⁷, a comparable sensitivity could be achieved with a single arm. Finally, we discuss the feasibility of achieving similar gravitational wave sensitivities in a `Doppler tracking' configuration where the single arm is anchored to Earth.34 pagesen-USAttribution 4.0 Internationalhttps://creativecommons.org/licenses/by/4.0/Astrophysics - Instrumentation and Methods for AstrophysicsGeneral Relativity and Quantum CosmologyAstrophysics - High Energy Astrophysical PhenomenaText