The stability and transport of carbon dioxide on Iapetus

Carbon dioxide has been detected associated with Iapetusʹ dark material by the Cassini spacecraft. This CO2 may be primordial and/or resulting from ongoing production by photolysis of water-ice in the presence of carbonaceous material [Allamandola, L.J., Sandford, S.A., Valero, G.J., 1988. Icarus 76, 225–252]. Although any primordial CO2 would likely be complexed with the dark material and thus stable against thermal transport to Iapetusʹ poles [Buratti, B.J., and 28 colleagues, 2005. Astrophys. J. 622, L149–L152], active production of CO2 would result in some fraction of the CO2 being mobile enough to allow the accumulation of CO2 at Iapetusʹ poles. We develop a computer model to simulate ballistic transport of CO2 ice on Iapetus, accounting for Iapetusʹ gravitational binding energy and polar cold traps. We find that the residence time of CO2 ice outside the polar regions is very short; a sheet of CO2 ice near the equator of Iapetus decreases in thickness at a rate of 50 mm year−1. The sublimated CO2 will ballistically move around Iapetus until it reaches the polar cold traps where it can be sequestered for up to 15 years. If the total surface inventory of CO2 exceeds 3 × 10 7 kg , the polar ice cap will be permanent. While CO2 is moving around the surface, a small percentage will eventually reach escape velocity and be lost from the system. As such, a seasonal polar cap is lost at rate of 12% every solar orbit as the CO2 moves between the two polar cold traps.