Velocity Distribution of CMEs After Projection Correction

Details Velocity Distribution of CMEs After Projection Correction Velocity Distribution of CMEs After Projection Correction

Apr 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010cha%26a..34..154g&link_type=abstract

Chinese Astronomy and Astrophysics, Volume 34, Issue 2, p. 154-162.

Astronomy and Astrophysics

Astrophysics

Scientific paper

The observed CME (coronal mass ejection) is its projection on the sky plane, and this leads to certain discrepancies between the observational and true parameters of the CME. For example, the observed velocity is generally smaller than the true velocity. The method of making projection correction for the CME velocity based on the conical model is utilized to analyze the velocity distributions of the 1691 CMEs which are only correlated to flares (called the class FL CMEs for short) and the 610 CMEs which are only correlated to filament eruptions (called the class FE CMEs for short) before and after the projection correction. These CMEs were observed with the Large Angle and Spectrometric Coronograph on the Solar and Heliospheric Observatory from September 1996 to September 2007 (close to a solar cycle). The obtained results are as follows: (1) before and after the projection correction the velocity distribution of FL CMEs is quite similar to that of FE CMEs, and before and after the projection correction the mean velocities of the two classes of CMEs are almost the same; (2) before and after the projection correction, the natural logarithm distribution of the FL CME velocities is also very similar to that of the FE CME velocities.

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