  Two major coronal mass ejections (CMEs) observed during the Whole Heliosphere
Interval (WHI) are compared with the catastrophe (CA) and eruptive flux rope
(EF) models. The objective is to test two distinct mechanisms for CMEs by
modeling these well-observed CMEs and comparing predictions of the theories and
observed data. The two CMEs selected for this study occurred on 25 March and 5
April 2008, respectively. For the 25 March event, an M 1.7 class flare, a
filament eruption, and hard X-ray (HXR) and soft X-ray (SXR) emissions were
observed during the CME onset. The observed CME kinematics and SXR light curve
of this event are found to be more consistent with the EF model than with the
CA model. For the 5 April event, the SXR light curve shows multiple
enhancements, some of which temporally coincide with successive side loop
brightening and multiple foot points at the source region after the eruption.
The physical connection between the side-loop multiple brightenings and the
eruption cannot be determined from the data. Both models produced
observationally consistent kinematics profiles, and the EF model correctly
predicted the first emission enhancement. Neither model includes multiple
brightenings in the formulation.
