Abstract
The Coronal Mass Ejections (CMEs) observed by the LASCO coronagraph and associated solar activity phenomena whose locations were identified by EIT and solar Hα flare observations during year 2000 indicate that about 40%, 26% and 30% of CMEs were observed when there were coronal holes (CHs) within 1–10, 11–20 and 21–40 degrees, respectively from the location of solar Hα flares. We are of the view, as also earlier suggested by Verma & Pande (1989) , that CMEs might have been produced by the same mechanism by which the mass ejected by the same solar flares or active prominences connects with open magnetic lines of CHs (source of high speed solar wind streams) and moves along them to appear as CMEs.
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