engleski

Projection effects in coronal mass ejections

Basic observational parameters of a Coronal Mass Ejection (CME) are its speed and angular width. Measurements of the CME speed and angular width are severely influenced by projection effects. The goal of this paper is to investigate a statistical relationship between the plane-of-sky speeds of CMEs and the direction of their propagation, hopefully providing an estimate of true speeds of CMEs. We analyze the correlation between the plane-of-sky velocity and the position of the CME source region, employing several non-halo CME samples. The samples are formed applying various restrictions to avoid crosstalk of relevant parameters. For example, we select only CMEs observed to radial distances larger than 10 solar radii ; we omit CMEs showing a considerable acceleration in the considered distance range ; we treat separately CMEs of different angular widths. Finally, we combine these restriction criteria, up to the limits beyond which the statistical significance of the results becomes ambiguous. A distinct anti-correlation is found between the angular width of CMEs and their source region position, clearly showing an increasing trend towards the disc center. Similarly, all of the considered subsamples show a correlation between the CME projected speed and the distance of the source region from the disc center. On average, velocities of non-halo limb-CMEs are 1.5\, --\, 2 times larger than in the case of non-halo CMEs launched from regions located close to the disc center. Unfortunately, the established empirical relationships provide only a rough estimate of the velocity correction as a function of the source region location. To a certain degree, the results can be explained in terms of CME cone-models, but only after taking into account crosstalk of various parameters and observational artifacts.

Sun - CMEs

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