Uranus has three known co-orbitals: 83982 Crantor (2002 GO9), 2010 EU65 and2011 QF99. Here, we perform a comparative analysis of the orbital evolution ofthese transient co-orbitals to understand better how they got captured in thefirst place and what makes them dynamically unstable. We also look foradditional temporary Uranian co-orbital candidates among known objects. OurN-body simulations show that the long-term stability of 2011 QF99 is controlledby Jupiter and Neptune; it briefly enters the 1:7 mean motion resonance withJupiter and the 2:1 with Neptune before becoming a Trojan and prior to leavingits tadpole orbit. During these ephemeral two-body mean motion resonanceepisodes, apsidal corotation resonances are also observed. For knownco-orbitals, Saturn is the current source of the main destabilizing force butthis is not enough to eject a minor body from the 1:1 commensurability withUranus. These objects must enter mean motion resonances with Jupiter andNeptune in order to be captured or become passing Centaurs. Asteroid 2010 EU65,a probable visitor from the Oort cloud, may have been stable for several Myrdue to its comparatively low eccentricity. In addition, we show that theorbital properties and discovery circumstances of known objects can be used tooutline a practical strategy by which additional Uranus' co-orbitals may befound.
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