  We compute the profiles of resonance doublet lines formed in bipolar winds
with velocity greater than the doublet separation in symbiotic stars.
Particular attention has been paid on the doublet line ratio, where the
conversion of the short wavelength component arising from the
$2S_{1/2}-2P_{3/2}$ transition into the long wavelengh component for the
transition $2S_{1/2}-2P_{1/2}$ plays an essential role in determining the flux
line ratio of the doublet. We adopted a Monte Carlo technique and the Sobolev
approximation. Our bipolar winds take the form of a cone and are characterised
by the terminal wind velocity, mass loss rate and the opening angle of the
cone. When the observer is in the polar direction and the Sobolev optical depth
is moderate $\tau_{Sob}\simeq 1$, then we mainly obtain profiles with inverted
flux line ratios, where the short wavelength component is weaker than the long
wavelength component. When the observer is in the equatorial direction, we find
that the profiles are characterised by two broad components, where the long
wavelength component is the broader and stronger of the two. We conclude that
the profiles obtained in our model provide qualitative understanding of broad
and inverted intensity ratio of the doublets in symbiotic stars and that the
bipolarity of the stellar winds can be inferred from the broader and stronger
long wavelength components in the doublet.
