Abstract
We use the recently determined rotation state, shape, size and thermophysical model of Apophis to predict the strength of the Yarkovsky effect in its orbit. Apophis does not rotate about the shortest principal axis of the inertia tensor, rather its rotational angular momentum vector wobbles at an average angle of similar or equal to 37 degrees from the body axis.
Therefore, we pay special attention to the modeling of the Yarkovsky effect for a body in such a tumbling state, a feature that has not been described in detail so far. Our results confirm that the Yarkovsky effect is not significantly weakened by the tumbling state.
The previously stated rule that the Yarkovsky effect for tumbling kilometer-size asteroids is well represented by a simple model assuming rotation about the shortest body axis in the direction of the rotational angular momentum and with rotation period close to the precession period is confirmed. Taking into account uncertainties of the model parameters, as well as the expected density distribution for Apophis' spectral class, we predict the secular change in the semimajor axis is (-12.8 +/- 3.6) x 10(-4) au/Myr (formal 1 cr uncertainty).
The currently available astrometric data for Apophis do not allow an unambiguous direct detection of the Yarkovsky effect. However, the fitted secular change in semimajor axis of (-23 +/- 13) x 10(-4) au/Myr is compatible with the model prediction.
We revise the Apophis' impact probability information in the second half of this century by extending the orbital uncertainty derived from the current astrometric data and by taking into account the uncertainty in the dynamical model due to the thermal recoil accelerations.