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The mass evolution of a coronal mass ejection (CME) is an important parametercharacterizing the drag force acting on a CME as it propagates throughinterplanetary space. Spacecraft measure in-situ plasma densities of CMEsduring crossing events, but for investigating the mass evolution, we also needto know the CME geometry, more specific, its volume. Having derived the CMEvolume and mass from remote sensing data using 3D reconstructed CME geometry,we can calculate the CME density and compare it with in-situ proton densitymeasurements near Earth. From that we may draw important conclusions on apossible mass increase as the CME interacts with the ambient solar wind in theheliosphere. In this paper we will describe in detail the method for derivingthe CME volume using the graduated cylindrical shell (GCS) model (Thernisien etal., 2006,2009, see Figure 1). We show that, assuming self-similar expansion,one can derive the volume of the CME from two GCS parameters and that itfurthermore can be expressed as a function of distance.

CME volume calculation from 3D GCS reconstruction