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In order to have a comprehensive view of the propagation and evolution ofcoronal mass ejections (CMEs) from the Sun to deep interplanetary space beyond1 au, we carry out a kinematic analysis of 7 CMEs in solar cycle 23. The eventsare required to have coordinated coronagraph observations, interplanetary typeII radio bursts, and multi-point in-situ measurements at the Earth and Ulysses.A graduated cylindrical shell model, an analytical model without freeparameters and a magnetohydrodynamic model are used to derive CME kinematicsnear the Sun, to quantify the CME/shock propagation in the Sun-Earth space, andto connect in-situ signatures at the Earth and Ulysses, respectively. We findthat each of the 7 CME-driven shocks experienced a major deceleration beforereaching 1 au and thereafter propagated with a gradual deceleration from theEarth to larger distances. The resulting CME/shock propagation profile for eachcase is roughly consistent with all the data, which verifies the usefulness ofthe simple analytical model for CME/shock propagation in the heliosphere. Thestatistical analysis of CME kinematics indicates a tendency that the faster theCME, the larger the deceleration, and the shorter the deceleration time periodwithin 1 au. For several of these events, the associated geomagnetic stormswere mainly caused by the southward magnetic fields in the sheath region. Inparticular, the interaction between a CME-driven shock and a preceding ejectasignificantly enhanced the preexisting southward magnetic fields and gave riseto a severe complex geomagnetic storm.

astrophysical journal/the astrophysical journal

Quantifying the Propagation of Fast Coronal Mass Ejections from the Sun  to Interplanetary Space Combining Remote Sensing and Multi-Point in-situ  Observations