In the recent ten years the problem of radial abundance gradients in spiral galaxies has emerged as a central problem in the field of galactic chemodynamics. Abundance gradients as observational characteristics of the galactic disc are among the most important input parameters in any theory of galactic chemical evolution. Further development of theories of galactic chemodynamics is dramatically hampered by the scarcity of observational data, their large uncertainties and, in some cases, apparent contradictions between independent observational results. Many questions concerning the present-day abundance distribution in the galactic disc, its spatial properties, and evolution with time, still have to be answered.

In present study, which concerns the elemental distribution in galactic disc based on Cepheids at galactocentric distances from 4 kpc to 11 kpc, the following results were obtained:

1. Using 241 high-resolution spectra of 83 galactic Cepheids the gradients for 25 chemical elements (from carbon to gadolinium) were derived.

2. Almost all investigated elements showed a rather flat abundance distributions in the middle part of galactic disc (distances from 6 kpc to 11 kpc). Typical values for iron-group elements lie within an interval from -0.02 to -0.04 dex/kpc (in particular, for iron we obtained -0.029 dex/kpc). Similar gradients were also obtained for O, Mg, Al, Si, and Ca.

3. For elements from Zr to Gd we obtained (within the error bar) zero gradients.

4. The gradient values obtained for the solar neighbourhood indicate that the radial abundance distribution within approximately 8 kpc +/- 2 kpc is quite homogeneous, and this result favours a galactic model including the bar structure which may induce radial flows in the disc, and thus may be responsible for abundance homogenization.