  Radial structure of accretion discs around compact objects is often described
using analytic approximations which are derived from averaging or integrating
vertical structure equations. For non-solar chemical composition, partial
ionization, or for supermassive black holes, this approach is not accurate.
Additionally, radial extension of `analytically-described' disc zones is not
evident in many cases. We calculate vertical structure of accretion discs
around compact objects, with and without external irradiation, with radiative
and convective energy transport taken into account. For this, we introduce a
new open Python code, allowing different equations of state (EoS) and opacity
laws, including tabular values. As a result, radial structure and stability
`S-curves' are calculated for specific disc parameters and chemical
composition. In particular, based on more accurate power-law approximations for
opacity in the disc, we supply new analytic formulas for the farthest regions
of the hot disc around stellar-mass object. On calculating vertical structure
of a self-irradiated disc, we calculate a self-consistent value of the
irradiation parameter $C_{\rm irr}$ for stationary $\alpha$-disc. We find that,
for a fixed shape of the X-ray spectrum, $C_{\rm irr}$ depends weakly on the
accretion rate but changes with radius, and the dependence is driven by the
conditions in the photosphere and disc opening angle. The hot zone extent
depends on the ratio between irradiating and intrinsic flux: corresponding
relation for $T_{\rm irr,\, crit}$ is obtained.
