Tuesday

The analysis of the deflection of coronal mass ejection (CME) events plays an important role in the improvement of the forecasting of their geo-effectiveness. To better understand the governing conditions of CME deflections we performed an exhaustive analysis of several events showing large deflections along a one-year time interval during the rising phase of solar cycle 24. We inspected the 3D trajectory of CMEs and the associated filaments with respect to their solar sources by means of a forward model and a tie-pointing tool, respectively. We applied these techniques to solar corona observations at different heights and wavelengths onboard PROBA2, SDO, STEREO and SOHO. Inspired by previous works, we analyse the influence of the magnetic energy density in the deflection of both structures using PFSS extrapolations. We determine the angle between the trajectory and the gradient of the magnetic energy density for the CMEs and for the associated filaments. In agreement with previous reports, most of the CME deflections are oriented with the direction of the magnetic energy decrease while for prominences the deflection seems to be related to the strength of the magnetic field. Through a kinematic analysis of both structures, we found a relation between the CME and filament speeds to the amount of deflection. For both structures, we also show that most of the deflection occurs at altitudes lower than 2.5 solar radii.