At a mean diameter of \sim 650 ~ { } m , the near-Earth asteroid ( 455213 ) 2001 OE84 ( OE84 for short ) has a rapid rotation period of 0.486542 \pm 0.000002 ~ { } hours , which is uncommon for asteroids larger than \sim 200 ~ { } m. We revisited OE84 14 years after it was first , and last , observed by Pravec et al . ( 2002 ) in order to measure again its spin rate and to search for changes . We have confirmed the rapid rotation and , by fitting the photometric data from 2001 and 2016 using the lightcurve inversion technique , we determined a retrograde sense of rotation , with the spin axis close to the ecliptic south pole ; an oblate shape model of a / b = 1.32 \pm 0.04 and b / c = 1.8 \pm 0.2 ; and no change in spin rate between 2001 and 2016 . Using these parameters we constrained the body ’ s internal strength , and found that current estimations of asteroid cohesion ( up to \sim 80 ~ { } Pa ) are insufficient to maintain an intact rubble pile at the measured spin rate of OE84 . Therefore , we argue that a monolithic asteroid , that can rotate at the rate of OE84 without shedding mass and without slowing down its spin rate , is the most plausible for OE84 , and we give constraints on its age , since the time it was liberated from its parent body , between 2 - 10 million years .