Evolution of coronal mass ejections in the inner heliosphere: A study using white-light and scintillation images

Knowledge of the radial evolution of the coronal mass ejection (CME) is important for the understanding of its arrival at the near-Earth space and of its interaction with the disturbed/ambient solar wind in the course of its travel to 1AU and further. In this paper, the radial evolution of 30 large CMEs ( angular width > 150 degrees, i. e., halo and partial halo CMEs) has been investigated between the Sun and the Earth using ( i) the white-light images of the near-Sun region from the Large Angle Spectroscopic Coronagraph (LASCO) onboard SOHO mission and (ii) the interplanetary scintillation (IPS) images of the inner heliosphere obtained from the Ooty Radio Telescope (ORT). In the LASCO field of view at heliocentric distances R <= 30 solar radii (R-.), these CMEs cover an order of magnitude range of initial speeds, V-CME approximate to 260 - 2600 km s(-1). Following results have been obtained from the speed evolution of these CMEs in the Sun - Earth distance range: ( 1) the speed profile of the CME shows dependence on its initial speed; ( 2) the propagation of the CME goes through continuous changes, which depend on the interaction of the CME with the surrounding solar wind encountered on the way; ( 3) the radial-speed profiles obtained by combining the LASCO and IPS images yield the factual view of the propagation of CMEs in the inner heliosphere and transit times and speeds at 1AU computed from these profiles are in good agreement with the actual measurements; ( 4) the mean travel time curve for different initial speeds and the shape of the radial-speed profiles suggest that up to a distance of similar to 80 R-., the internal energy of the CME ( or the expansion of the CME) dominates and however, at larger distances, the CME's interaction with the solar wind controls the propagation; ( 5) most of the CMEs tend to attain the speed of the ambient flow at 1AU or further out of the Earth's orbit. The results of this study are useful to quantify the drag force imposed on a CME by the interaction with the ambient solar wind and it is essential in modeling the CME propagation. This study also has a great importance in understanding the prediction of CME-associated space weather at the near-Earth environment.