  Calculations of the expected TeV $\gamma$-ray emission, produced by
accelerated cosmic rays (CRs) in nuclear collisions, from supernova remnants
evolving in a uniform interstellar medium (ISM) are presented. The aim is to
study the sensitivity of $\gamma$-ray production to a physical parameter set.
Apart from its general proportionality to N_H, it is shown that the
$\gamma$-ray production essentially depends upon the ratio of the CR diffusion
coefficient $\kappa$ to a critical value $\kappa_{crit}=10(B_0/5
\mu{G})(N_H/0.3 {cm}^{-3})^{-1/3}\kappa_B$, where B_0 and N_H are the magnetic
field and hydrogen number density of the ISM, and $\kappa_B$ denotes the Bohm
diffusion coefficient. If $\kappa$ is of the same order or lower than
$\kappa_{crit}$, then the peak TeV $\gamma$-ray flux in the Sedov evolutionary
phase, normalized to a distance of 1 kpc, is about 10^{-10}(N_H/0.3 {cm}^{-3})
photons cm^{-2} s^{-1}. For a CR diffusion coefficient that is significantly
larger than $\kappa_{crit}$, the CR cutoff energy is less than 10 TeV and the
expected $\gamma$-ray flux at 1 TeV is considerably below the presently
detectable level of 10^{-12} photons cm^{-2} s^{-1}. The same is of course true
for a SNR in the rarified, so-called hot ISM.
