Physical Considerations for an Intercept Mission to a 1I/’Oumuamua-Like Interstellar Object

Abstract

In this paper, we review some of the extant literature on the study of interstellar objects (ISOs). With the forthcoming Vera C. Rubin Telescope and Legacy Survey of Space and Time (LSST), we find that 0.38−84 'Oumuamua-like interstellar objects are expected to be detected in the next 10 years, with 95% confidence. The feasibility of a rendezvous trajectory has been demonstrated in previous work. In this paper, we investigate the requirements for a rendezvous mission with the primary objective of producing a resolved image of an interstellar object. We outline the rendezvous distances necessary as a function of resolution elements and object size. We expand upon current population synthesis models to account for the size dependency on the detection rates for reachable interstellar objects. We assess the trade-off between object diameter and occurrence rate, and conclude that objects with the size range between a third of the size and the size of 'Oumuamua will be optimal targets for an imaging rendezvous. We also discuss expectations for surface properties and spectral features of interstellar objects, as well as the benefits of various spacecraft storage locations.

Chasing nomadic worlds: A new class of deep space missions

“…While this choice of 𝐷 𝑖 ∼ 𝐷 ISO constitutes an idealization to some degree, it might not be unreasonable provided that the detection occurs at distances ≳ 𝐷 ISO when the ISO is inbound into the Solar system and the spacecraft is designed and equipped beforehand for a quick launch thereafter [refer to 121, Section 5.5.4]. Plausible mission architectures to intercept ISOs of sizes ≲ 1-10 km based on different wait times, orbital maneuvers, and propulsion methods have been formulated by many authors [122,123,124,125,126,127,128,129,130,131,132,133,134,135,136,137].…”

“…This relation means that it should be possible to distinguish immediately between bound objects (with orbital velocities of a few km/s or less) and unbound ISOs, with typical SSB velocities of several tens of km/s [10,144,94,135]. The dynamical observables (two components each of position and velocity) that can be computed from a single occultation are not enough, of course, to fully determine the orbit of the newly discovered object.…”

“…2. The hyperbolic excess velocities (𝑣 ∞ ) of most ISOs are ostensibly few/several tens of km/s [see, e.g., 10,144,94,135]. As long as the perihelia of these ISOs are not close to the Sun, it is reasonable to suppose that 𝐯 ISO is on the order of 𝑣 ∞ throughout.…”