Possible paths of Venus’s spin pole in the BRF over 12 000 years, showing less than one period of the Chandler wobble. The motion corresponds to Eq. (40) for a liquid outer core. The thirty green dots show possible initial positions of the pole at epoch J2000. The red dots show the positions after 12 000 years, their spread reflecting the Chandler period range from Eq. (42). Fluctuations due to high-frequency forcing are too small to be seen at this scale (see Fig. 5).