  YORP-induced fission events may form dynamically coherent pairs or even
families of asteroids. The outcome of this process is well documented among
members of the main asteroid belt, but not in the case of the near-Earth
asteroid (NEA) population because their paths randomize very efficiently in a
short time-scale. Mean-motion resonances (MMRs) may stabilize the orbits of
small bodies by making them avoid close encounters with planets. In theory,
YORP-induced fission of asteroids trapped in MMRs can preserve evidence of this
process even in near-Earth space. Here, we show that two NEAs, 2017 SN16 and
2018 RY7, are currently following an orbital evolution in which their relative
mean longitude does not exhibit any secular increase due to the stabilizing
action of the 3:5 MMR with Venus. The mechanism that makes this configuration
possible may be at work both in the Solar system and elsewhere. Our analysis
suggests that the pair 2017 SN16-2018 RY7 may have had its origin in one out of
two mechanisms: YORP-induced splitting or binary dissociation.
