  A number of modern experiments in high-energy astrophysics produce images of
supernova remnants (SNRs) in the TeV and GeV gamma-rays. Either relativistic
electrons (due to the inverse-Compton scattering) or protons (due to the pion
decays) may be responsible for this emission. In particular, the broad-band
spectra of SNRs may be explained in both leptonic and hadronic scenarios.
Another kind of observational data, namely, images of SNRs, is an important
part of experimental information. We present a method to model gamma-ray images
of Sedov SNRs in uniform media and magnetic field due to hadronic emission.
These gamma-rays are assumed to appear as a consequence of meson decays
produced in inelastic collisions of accelerated protons with thermal protons
downstream of the shock - a model would be relevant for SNRs without firm
confirmations of the shock-cloud interaction, as e.g. SN1006. Distribution of
surface brightness of the shell-like SNR is synthesized numerically for a
number of configurations. An approximate analytical formula for azimuthal and
radial variation of hadronic gamma-ray brightness close to the shock is
derived. The properties of images as well as the main factors determining the
surface brightness distribution are determined. Some conclusions which would be
relevant to SN1006 are discussed.
