  We investigated flow in Schwarzschild metric, around a non-rotating black
hole and obtained self-consistent accretion - ejection solution in full general
relativity. We covered the whole of parameter space in the advective regime to
obtain shocked, as well as, shock-free accretion solution. We computed the jet
streamline using von - Zeipel surfaces and projected the jet equations of
motion on to the streamline and solved them simultaneously with the accretion
disc equations of motion. We found that steady shock cannot exist {for $\alpha
\gsim0.06$} in the general relativistic prescription, but is lower if mass -
loss is considered too. We showed that for fixed outer boundary, the shock
moves closer to the horizon with increasing viscosity parameter. The mass
outflow rate increases as the shock moves closer to the black hole, but
eventually decreases, maximizing at some intermediate value of shock
{location}. The jet terminal speed increases with stronger shocks,
quantitatively speaking, the terminal speed of jets $v_{{\rm j}\infty} > 0.1$
if $\rsh < 20 \rg$. The maximum of the outflow rate obtained in the general
relativistic regime is less than $6\%$ of the mass accretion rate.
