Time lag of the dayside magnetosphere's response to large changes in the solar wind He++/H+ ratio

Solar wind is injected into Earth's magnetosphere via reconnection at either low latitudes or high latitudes, flows into the magnetotail plasma sheet, is driven Earthward by tail reconnection, and ultimately becomes part of the ring current. The time it takes for solar wind ions to enter the magnetosphere and convect back to the dayside is referred to as the convection time lag. Using data from the Advanced Composition Explorer (ACE), Magnetospheric Multiscale (MMS), and WIND spacecraft, we examine a number of solar wind events in 2015 where the He++/H+density ratio experienced large changes (greater than 0.1) over the course of a few hours. We calculate the He++/H+density ratio in the magnetosphere in the aftermath of these events and correlate these magnetospheric composition structures with previously observed structures in the solar wind in order to determine the convection time lag.