  This work provides analytical solutions describing the post-shock structure
of radiative shocks growing in astrophysics and in laboratory. The equations
including a cooling function $\Lambda \propto \rho^{\epsilon} P^{\zeta}
x^{\theta}$ are solved for any values of the exponents $\epsilon$, $\zeta$ and
$\theta$. This modeling is appropriate to astrophysics as the observed
radiative shocks arise in optically thin media. In contrast, in laboratory,
radiative shocks performed using high-power lasers present a radiative
precursor because the plasma is more or less optically thick. We study the
post-shock region in the laboratory case and compare with astrophysical shock
structure. In addition, we attempt to use the same equations to describe the
radiative precursor, but the cooling function is slightly modified. In future
experiments we will probe the PSR using X-ray diagnostics. These new
experimental results will allow to validate our astrophysical numerical codes.
