Eclipses by Artificial Satellites to Measure the Angular Sizes of Stars

Direct measurements of the angular sizes of stars (other than our Sun) are inherently limited by telescopes’ optical diffraction limit. The spatial diffraction limit can be overcome by using time-domain information when stars are eclipsed' by anything moving in the foreground: artificial satellites or the Moon (known as lunar occultation imaging’). Here we analyse the angular resolution achievable by high-speed photon counting devices, when stars are eclipsed for several microseconds by one of the thousands of satellites now in low or mid-Earth orbit. We also build a full Bayesian statistical treatment for analysing simulated observations. We show that eclipses by the moon and satellites deliver $<2$ milliarcsecond resolution for $\sim$${10}^4$ stars every year, with the diameters of $\sim$${10}^1-{10}^2$ stars constrained to better than $0.5$ milliarcseconds. The application of satellites requires an ultra-fast, photon-resolving detector, capable of continuous readout with inter-frame delay controlled within $\lesssim 1$ $\mu$s. Such a fast rate can easily be handled by the SPINA instrument, which has demonstrated $8$ ns inter-frame delay, and potentially by the Cherenkov Telescope Array.