  Analysis of the solar coronal green line profiles reveals information
regarding the physical conditions of the solar corona like temperature,
density, Doppler velocity, non-thermal velocity etc. It provides insights to
the unresolved problems like the coronal heating and the acceleration of the
solar winds. Recent studies have reported excess blueshifts in the coronal line
profiles and are interpreted as due to nanoflare heating, type II spicules and
nascent solar wind flow. We have analyzed a time series of Fabry-Perot
interferograms of the solar corona obtained during the total solar eclipse of
2001 June 21 from Lusaka, Zambia. The spatial behavior of the coronal green
line profiles were examined and variations in intensity, linewidth, Doppler
velocity and line asymmetry were obtained. Several line profiles showed
asymmetry indicating the presence of multicomponents. Such line profiles were
fitted with double Gaussian curves. It has been found that 42% of the line
profiles were single components, 34% were blueshifted, and 24% were red
shifted. The secondary component of a typical line profile with blue asymmetry
is found to have a relative intensity about 0.26, Doppler velocity around -30
km/s and a halfwidth about 0.65A.
