by @wilkin96. Other approximations, such as the Bohm diffusion in the shock vicinity, and a parametrization of the magnetic field amplification (MFA) due to CR-driven instabilities, are the same as in @MNRAS_BGO13. The reader is referred to that paper for full details. Our results for neutrino and [$\gamma$-ray]{} production in , given in Section \[sec:WestI\], use our [nonlinear]{}, time-dependent model. However, to describe the general characteristics of , we shall start in this section with simple analytic estimates from a linear model in a plain-parallel case [e.g., @bgo11]. Considering a SNR expanding in a compact OB-association; at some expansion phase the distance $L$ between the SNR blast wave and a stellar wind shock is less than the mean free path of the highest energy CRs in the SNR shock precursor. At this point, the CR distribution function around the two shocks, indicated by $i = 1,2$, can be approximated as $$\label{SolveDC}
\begin{array}{l}
 f_i \left( {x,p,t} \right)= A p^{-3}\exp \left( {-\frac{u_i }{D_i }\left| x \right|}
\right)\times \\
\times  H\left( {p-p_0 } \right)H\left( {t- {t_\mathrm{acc}}} \right)
\ ,
\end{array}$$ where the CR acceleration time is $$\label{TauAc}
{t_\mathrm{acc}}=\int\limits_{p_0 }^p {\frac{3}{\left( {u_1 +u_2 }
\right)}\left( {\frac{D_1 }{u_1 }+\frac{D_2 }{u_2 }} \right)}
\frac{dp}{p}.$$ It is 