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We study the interaction of two successive coronal mass ejections (CMEs)during the 2010 August 1 events using STEREO/SECCHI COR and HI data. We obtainthe direction of motion for both CMEs by applying several independentreconstruction methods and find that the CMEs head in similar directions. Thisprovides evidence that a full interaction takes place between the two CMEs thatcan be observed in the HI1 field-of-view. The full de-projected kinematics ofthe faster CME from Sun to Earth is derived by combining remote observationswith in situ measurements of the CME at 1 AU. The speed profile of the fasterCME (CME2; ~1200 km/s) shows a strong deceleration over the distance range atwhich it reaches the slower, preceding CME (CME1; ~700 km/s). By applying adrag-based model we are able to reproduce the kinematical profile of CME2suggesting that CME1 represents a magnetohydrodynamic obstacle for CME2 andthat, after the interaction, the merged entity propagates as a single structurein an ambient flow of speed and density typical for quiet solar windconditions. Observational facts show that magnetic forces may contribute to theenhanced deceleration of CME2. We speculate that the increase in magnetictension and pressure, when CME2 bends and compresses the magnetic field linesof CME1, increases the efficiency of drag.

Characteristics of kinematics of a coronal mass ejection during the 2010 August 1 CME-CME interaction event