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Studying the evolution of magnetic clouds entrained in coronal mass ejectionsusing in-situ data is a difficult task since only a limited number ofobservational points is available at large heliocentric distances. Remotesensing observations can, however, provide important information for eventsclose to the Sun. In this work we estimate the flux rope orientation first inthe close vicinity of the Sun (2-20 Rs) using forward modeling of STEREO/SECCHIand SOHO/LASCO coronagraph images of coronal mass ejections and then in-situusing Grad-Shafranov reconstruction of the magnetic cloud. Thus, we are able tomeasure changes in the orientation of the erupted flux ropes as they propagatefrom the Sun to 1 AU. We present both techniques and use them to study 15magnetic clouds observed during the minimum following Solar Cycle 23 and therise of Solar Cycle 24. This is the first multievent study to compare thethree-dimensional parameters of CMEs from imaging and in-situ reconstructions.The results of our analysis confirm earlier studies showing that the flux ropestend to deflect towards the solar equatorial plane. We also find evidence ofrotation on their travel from the Sun to 1 AU. In contrast to past studies, ourmethod allows one to deduce the evolution of the three-dimensional orientationof individual flux ropes rather than on a statistical basis.

Three-dimensional evolution of erupted flux ropes from the Sun (2-20 Rs) to 1 AU