Can coronal mass ejections reverse the open field polarity over the solar cycle?

It has recently been demonstrated that the solar cycle variation in the total unsigned magnetic flux in the heliosphere can be explained by the temporary build-up of closed flux released by coronal mass ejections (CMEs). The closed flux within Interplanetary-CMEs is assumed to eventually open via interchange reconnection close to the Sun. Throughout this process the total amount of open flux on the Sun is conserved, though a reconfiguration of the open flux is expected. Each eruption of a CME moves the interchanged open flux by the CME foot-point separation distance. We demonstrate that the amount of flux transported by CME eruptions and subsequent interchange reconnection is adequate to account for the polar field reversal over the 11 year solar cycle. However, for such CME flux transport to be a viable mechanism for the solar cycle field reversal, the polarity of the CME flux opened by interchange reconnection must follow a very systematic pattern. Initial in situ observations of magnetic clouds suggest this to be the case.