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The YORP effect is a small thermal-radiation torque experienced by smallasteroids, and is considered to be crucial in their physical and dynamicalevolution. It is important to understand this effect by providing measurementsof YORP for a range of asteroid types to facilitate the development of atheoretical framework. We are conducting a long-term observational study on aselection of near-Earth asteroids to support this. We focus here on (68346)2001 KZ66, for which we obtained both optical and radar observations spanning adecade. This allowed us to perform a comprehensive analysis of the asteroid'srotational evolution. Furthermore, radar observations from the AreciboObservatory enabled us to generate a detailed shape model. We determined that(68346) is a retrograde rotator with its pole near the southern ecliptic pole,within a $ 15^\circ$ radius of longitude $ 170^\circ$ and latitude $-85^\circ$. By combining our radar-derived shape model with the optical lightcurves we developed a refined solution to fit all available data, whichrequired a YORP strength of $ (8.43\pm0.69)\times10^{-8} \rm~rad ~day^{-2} $.(68346) has a distinct bifurcated shape comprising a large ellipsoidalcomponent joined by a sharp neckline to a smaller non-ellipsoidal component.This object likely formed from either the gentle merging of a binary system, orfrom the deformation of a rubble pile due to YORP spin-up. The shape exists ina stable configuration close to its minimum in topographic variation, whereregolith is unlikely to migrate from areas of higher potential.

Detection of the YORP Effect on the contact-binary (68346) 2001 KZ66 from combined radar and optical observations