Neglecting the terms associated with $f(\tilde s_0)$, the trilinear term can be calculated as

$$\label{trilinear}
\begin{split}
&A_{\alpha \beta \gamma} \simeq 
\frac{1}{M_p^2}~\frac{e^{h(\tilde t_0)/2}}{\tilde s_0^{1/2} \tilde t_0^{3/2}}~ s_0^{2}
~\left(f'(\tilde s_0) -\frac{\hat W}{2 \tilde s_0}\right)\left[-\frac{1}{2 \tilde{s}_0}
+\left(\partial_{\tilde{s}} \log Y_{\alpha \beta \gamma}\right)|_{VEV}\right].
\end{split}$$

Using the constraint (\[const2\]) and the expression for the gravitino mass (\[gravitino\]) this simplifies to, $$\label{trilinear2}
A_{\alpha \beta \gamma} \simeq  m_{3/2} \tilde{s}_0\left[-\frac{1}{2 \tilde{s}_0}
+\left(\partial_{\tilde{s}} \log Y_{\alpha \beta \gamma}\right)|_{VEV}\right].$$ Similarly the bilinear coupling reduces to,

$$\label{bilinear}
B \simeq m_{3/2} \tilde{s}_0 \left[-\frac{1}{2 \tilde{s}_0} + \partial_{\tilde{s}} \log \mu|_{VEV} \right]-m_{3/2}.$$

It can therefore be concluded that the trilinear (\[trilinear2\]) and bilinear parameters (\[bilinear\]) are also $\sim \rm TeV$. Thus following the discussion in sections (2),(3) and (4) it is easy to infer that the inclusion of an additional moduli field which breaks the susy may produce small vacuum energy in the hidden sector. The correction term is crucial to determine the nature of the minimum. The susy breaking parameters at the observable sector have the TeV scale values. In the following section an example in support of the above proposal is presented.

A toy model
===========

We construct a specific model to illustrate the general scenario discussed so far. It has already been mentioned that 