  The coronal green line (Fe XIV 5303 A) profiles were obtained from
Fabry-Perot interferometric observations of the solar corona during the total
solar eclipse of 21 June 2001 from Lusaka, Zambia. The instrumental width is
about 0.2 A and the spectral resolution is about 26000. About 300 line profiles
were obtained within a radial range of 1.0-1.5 R\odot and position angle
coverage of about 240\circ. The line profiles were fitted with single Gaussian
and their intensity, Doppler velocity, and line width have been obtained. Also
obtained are the centroids of the line profiles which give a measure of line
asymmetry. The histograms of Doppler velocity show excess blueshifts while the
centroids reveal a pre-dominant blue wing in the line profiles. It has been
found that the centroids and the Doppler velocities are highly correlated. This
points to the presence of multiple components in the line profiles with an
excess of blueshifted components. We have then obtained the(Blue-Red) wing
intensity which clearly reveals the second component, majority of which are
blueshifted ones. This confirms that the coronal green line profiles often
contain multicomponents with excess blueshifts which also depend on the solar
activity. The magnitude of the Doppler velocity of the secondary component is
in the range 20-40 km s-1 and they show an increase towards poles. The possible
explanations of the multicomponents could be the type II spicules which were
recently found to have important to the coronal heating or the nascent solar
wind flow, but the cause of the blue asymmetry in the coronal lines above the
limb remains unclear.
