Self-Consistent Evolution Models for Slow CMEs up to 1 AU

Our 2.5D (axi-symmetric) self-consistent numerical magneto-hydrodynamics (MHD) models for the onset of CMEs under solar minimum conditions and for their interaction with coronal streamers and subsequent evolution up to 1 AU, are presented and discussed. The CMEs are initiated by magnetic flux emergence/cancellation and/or by shearing the magnetic foot points of a magnetic arcade which is positioned above or below the equatorial plane and embedded in a larger helmet streamer. The overlying magnetic streamer field then deflects the CMEs towards the equator, and the deflection path is dependent on the driving velocity. The core of the CME, created during the onset process, contains a magnetic flux rope and the synthetic white light images often show the typical three-part CME structure. The resulting CMEs propagate only slightly faster than the background solar wind, but this small excess speed is high enough to create a fast MHD shock wave from a distance of 0.25 AU onwards. At 1 AU, the plasma shows the typical characteristics of a magnetic cloud, and the simulated data are in good agreement with the (ACE) observations.