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A coronal mass ejection is an expulsion of plasma and embedded magnetic field from the solar corona into interplanetary space. It carries matter as well as magnetic structure. A solar flare instead denotes a rapid atmospheric energy-release event observed through enhanced radiation; the two phenomena can accompany the same eruption without being interchangeable.^[ref]

A coronagraph suppresses the bright solar disc so that much fainter coronal structures can be followed outward. A sequence of images gives projected size, motion and morphology. SOHO's LASCO observations provide an important example of the instrument-based diagnosis used in space-weather analysis.^[ref]

For an illustrative measurement, suppose an apparent front moves from projected radius $3R_{\odot }$ to $7R_{\odot }$ in one hour. Using $R_{\odot }\simeq 6.96\times 10^8\mathrm{m}$ givesThis is a plane-of-sky speed, not automatically the true radial speed. Projection, the choice of visible front and evolution between frames affect the inference. Motion mainly towards the observer can produce a surrounding halo in projection rather than a simple sideward trajectory.

A passing interplanetary disturbance can also be studied through local solar wind density, velocity and magnetic-field measurements. A leading shock wave and the magnetized ejecta are different parts of that disturbance. Combining remote imaging with local measurements is more informative than treating brightness or apparent speed alone as a complete description of the eruption.