We have calculated Stark widths and shifts of some infrared helium lines th
at are missing and that are important for modellisation of the atmospheres
of hot early-type stars. These calculations are based on the impact and qua
sistatic theory and semi-classical approximation. The provided data are dis
played for a grid of temperatures (10(4) to 10(5) K) and electron densities
(10(10) to 10(13) cm(-3)) typical of hot early-type stars. We also discuss
the conditions of use of our data for astrophysical purposes.