Author(s): , , ,
Institution(s): 1. University of Michigan, 2. University of New Hampshire
Coronal mass ejections (CMEs) are the most energetic events from the Sun and the major driver of intense geomagnetic activity. Traditionally, most research has focused on understanding the causes of CME initiation and the specificities of the interaction between CMEs and Earth's magnetosphere. In-between these two domains, CMEs propagate in the heliosphere, interacting with the solar wind and other transient and corotating structures. The heliospheric propagation of CMEs can now be directly imaged remotely, making it possible to directly compare solar and coronal properties with CME properties measured in situ near Earth. In addition, numerical simulations can be used to get a more complete, 3-D view of CMEs. Here, I will review progress made in the past decade in our understanding of CME propagation and how it affects the CME properties as measured near Earth. In particular, I will discuss CME radial expansion, CME deflection and rotation as well as the interaction of successive CMEs and the interaction of a CME with corotating solar wind structures.