  With reasonable assumptions and approximations, we compute the velocity of
the meridional flow $U$ in the convective envelope by modified Chandrasekhar's
(1956) MHD equations. The analytical solution of such a modified equation is
found to be $U(x,\mu) = \sum_{n=0}^\infty \bigl[u1_n x^n + u2_n
x^{-(n+3)}\bigr] C_n^{3/2}(\mu)$, where $x$ is non-dimensional radius, $\mu =
cos{\vartheta}$, ${\vartheta}$ is the co-latitude, $C_n^{3/2} {(\mu)}$ are the
Gegenbaur polynomials of order 3/2, $u1_n$ and $u2_n$ are the unknown
constants. The results show that meridional velocity flow from the surface
appears to penetrates deep below base of the convective envelope and at outer
part of the radiative zone. With such a deep flow velocity below the convective
envelope and a very high density stratification in the outer part of the
radiative zone with likely existence of a strong ($\sim$ $10^{4}$ G) toroidal
magnetic field structure, the velocity of transport of meridional flow is
considerably reduced. Hence, it is very unlikely that the return flow will
reach the surface (with a period of solar cycle) as required by some of the
flux transport dynamo models. On the other hand, deep meridional flow is
required for burning of Lithium at outer part of the radiative zone supporting
the observed Lithium deficiency at the surface.
