Recent discoveries show that asteroids spinning in less than a few minutes undergo sizeable semi-major axis drifts, possibly driven by the Yarkovsky effect. Analytical formulas can match these drifts only if very low thermal inertia is assumed, implying a dust-fine regolith or a highly porous interior that is difficult to retain under such extreme centrifugal forces. With analytical theories of the Yarkovsky effect resting on a set of assumptions, their applicability to cases of super-fast rotation should be verified. We aim to evaluate the validity of the analytical models in such scenarios and to determine whether the Yarkovsky effect can explain the observed drift in rapidly rotating asteroids. We have developed a numerical model of the Yarkovsky effect tailored to super-fast rotators. The code resolves micrometer-scale thermal waves on millisecond time steps, capturing the steep gradients that arise when surface thermal inertia is extremely low. A new 3D heat-conduction and photon-recoil solver was benchmarked against the THERMOBS thermophysical code and the analytical solution of the Yarkovsky effect, over a range of rotation periods and thermal conductivities. The analytical Yarkovsky drift agrees well with the numerical solver. For thermal conductivities from 0. 0001 to 1 mathrm W m^ K^ and spin periods as short as 10 s, the two solutions differ by no more than 15%. This confirms that the observed semi-major axis drifts for super-fast rotators can be explained by the Yarkovsky effect and very low thermal inertia. Applied to the 34-s rapid rotator 2016 GE1, the best match of the measured drift was obtained with Gammałesssim20 mathrm J m^ K^ s^ a value that implies ∼100 K temperature swings each spin cycle. Analytical Yarkovsky expressions remain reliable down to spin periods of a few tens of seconds. The drifts observed in super-fast rotators require low-Γ surfaces and might point to rapid thermal fatigue as a regolith-generation mechanism.
Mar et al. (Sun,) studied this question.