On the full kinematic evolution of CMEs from the Sun to the Earth

We present a synthesis of the full kinematic evolution of CMEs from the Sun to the Earth. A CME is a large-scale magnetized-structure of plasma initiated close to the surface of the Sun. A CME undergoes multiple phases of distinct evolution that are controlled by unique dynamic process, including (1) a slow rising phase near the photospheric polarity inversion line, (2) an impulsive acceleration phase in the inner corona, (3) a gradual acceleration/deceleration phase in the outer corona, and (4) a propagation phase in the inner heliosphere. Using a few well observed events whose kinematic evolutions are fully and accurately constrained by observations from multiple spacecraft, including from SDO, SOHO and STEREO, we present multiple-phase-composite parametric formulae to model the evolution. The characterization of the evolution reveals the dynamic forces and their interplay that act on CME structures, including Lorentz self-force, external Lorentz force, gravitational force and aero-dynamic drag force. We will also discuss the similarity and difference of the evolution between CME ejecta and CME-driven shocks. The ultimate goal is to provide an accurate prediction model of CME arrival at the Earth.