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We have studied two coronal mass ejections (CMEs) that occurred on 25 and 28 September 2012 and interacted near the Earth. By fitting the Graduated Cylindrical Shell model on the SECCHI/COR2 images and applying the Stereoscopic Self‐Similar Expansion method on the SECCHI/HI images, the initial direction of both the CMEs is estimated to be west of the Sun‐Earth line. Further, the three‐dimensional (3‐D) heliospheric kinematics of these CMEs have been estimated using Self‐Similar Expansion (SSE) reconstruction method. We show that the use of SSE method with different values of angular extent of the CMEs leads to significantly different kinematics estimates for the CMEs propagating away from the observer. Using the estimated kinematics and true masses of the CMEs, we have derived the coefficient of restitution for the collision which is found to be close to elastic. The in situ measurements at 1 AU show two distinct structures of interplanetary CMEs, heating of the following CME, and ongoing interaction between the preceding and the following CME. We highlight the signatures of interaction in remote and in situ observations of these CMEs and the role of interaction in producing a major geomagnetic storm.

Kinematics of interacting CMEs of 25 and 28 September 2012