We study the relationship between magnetic reconnection and acceleration of filaments and coronal mass ejections (CMEs) in different magnetic configurations. They occur in either quiet-Sun or active regions of either bipolar or multipolar magnetic fields, and are either or not accompanied by filament eruptions. The preliminary results of the case studies confirm the temporal correlation and magnitude scaling relationship between reconnection rate and acceleration in the early phase of eruptions. The results suggest no clear difference between events of different magnetic configurations. It is shown that the total reconnection flux, which is calculated to be 10 21-22 Mx, is proportional to the average velocities of CMEs, suggesting the important role of magnetic reconnection in the early stage of solar eruptions.