Oumuamua (I1 2017) was the first macroscopic body observed to traverse the inner Solar System on an unbound hyperbolic orbit, making it the first interstellar object ever detected up close. `Oumuamua’s light curve displayed strong periodic variation, and it showed no hint of a coma or emission from molecular outgassing. Astrometric measurements indicate that `Oumuamua experienced non-gravitational acceleration on its outbound trajectory, but energy balance arguments indicate this acceleration is inconsistent with a water ice sublimation-driven jet. In the first part of this talk, I will show that all of `Oumaumua's observed properties can be explained if it contained a significant fraction of molecular hydrogen ice. I show that H2-rich bodies plausibly form in the coldest dense cores of Giant Molecular Clouds. I assess the near-term prospects for detecting and observing (both remotely and in-situ) future solar system visitors of this type. In the second part of this talk, I investigate the dynamical transfer of Centaurs into the inner Solar System, facilitated by mean motion resonances with Jupiter and Saturn. The recently discovered object, P/2019 LD2, will transition from the Centaur region to the inner Solar System in 2063. In order to contextualize LD2, I perform N-body simulations of a population of Centaurs and JFCs. The simulations show that there may be additional LD2-like objects transitioning into the inner Solar System in the near-term future, all of which have low ΔV with respect to Jupiter. I demonstrate that a spacecraft stationed near Jupiter would be well-positioned to rendezvous, orbit match, and accompany LD2 into the inner Solar System, providing an opportunity to observe the onset of intense activity in a pristine comet in situ.