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Our major aim is a height-time model $r(t)$ of the propagation of {\slCoronal Mass Ejections (CMEs)}, where the lower corona is self-consistentlyconnected to the heliospheric path. We accomplish this task by using theNeupert effect to derive the peak time, duration, and rate of the CMEacceleration phase, as obtained from the time derivative of the {\sl soft X-ray(SXR)} light curve. This novel approach offers the advantage to obtain thekinematics of the CME height-time profile $r(t)$, the CME velocity profile$v(t)=dr(t)/dt$, and the CME acceleration profile $a(t)=dv(t)/dt$ from {\slGeostationary Orbiting Earth Satellite (GOES)} and white-light data, withoutthe need of {\sl hard X-ray (HXR)} data. We apply this technique to a data setof 576 (GOES X and M-class) flare events observed with GOES and the {\sl LargeAngle Solar Coronagraph (LASCO)}. Our analysis yields acceleration rates in therange of $a_A = 0.1-13$ km s$^{-2}$, acceleration durations of $\tau_A =1.2-45$ min, and acceleration distances in the range of $d_A = 3-1063$ Mm, witha median of $d_A=39$ Mm, which corresponds to the hydrostatic scale height of acorona with a temperature of $T_e \approx 0.8$ MK. The results are consistentwith standard flare/CME models that predict magnetic reconnection andsynchronized (primary) acceleration of CMEs in the low corona (at a height of~0.1 R_sun), while secondary (weaker) acceleration may occur further out atheliospheric distances.

Global energetics of solar flares. XIII. The Neupert effect and acceleration of coronal mass ejections