  We constructed a comprehensive model atom for NeI -- NeII using the most
up-to-date atomic data available and evaluated the non-local thermodynamic
equilibrium (NLTE) line formation for NeI and NeII in classical 1D models
representing the atmospheres of B-type stars. We find that the large NLTE
strengthening of the NeI lines corresponding to the 2p$^5$3p $-$ 2p$^5$3s
transitions array occurs due to extremely small photoionization cross-sections
of 2p$^5$3s levels that leads to strong overpopulation of these levels relative
to their LTE populations. The deviations from LTE for the most NeII lines are
small and do not exceed 0.11~dex in the absolute value. We analysed 20 lines of
NeI and 13 lines of NeII for twenty-four B-type stars in the temperature range
of 10\,400 $\le$ \Teff\ $\le$ 33\,400~K. For five stars, the NLTE leads to
consistent abundances of NeI and NeII, while the difference in LTE abundance
can reach up to 0.50~dex. The using of the experimental oscillator strengths
recently measured by Piracha et al. (2015) leads to smaller line-by-line
scatter for the most investigated stars. The averaged neon abundance in
twenty-four B-type stars in solar neighborhood is 8.02$\pm$0.05. This value may
provide indirect constraints on solar photospheric neon abundance.
