Neon abundances in normal late-B and mercury-manganese stars

We make new non-local thermodynamic equilibrium calculations to deduce the abundances of neon from visible-region echelle spectra of selected Ne I lin es in seven normal stars and 20 HgMn stars. We find that the best strong bl end-free Ne line that can be used at the lower end of the effective tempera ture T-eff range is lambda 6402, although several other potentially useful Ne I lines are found in the red region of the spectra of these stars. The m ean neon abundance in the normal stars (log A=8.10) is in excellent agreeme nt with the standard abundance of neon (8.08). However, in HgMn stars neon is almost universally underabundant, ranging from marginal deficits of 0.1- 0.3 dex to underabundances of an order of magnitude or more. In many cases, the lines are so weak that only upper limits can be established. The most extreme example found is upsilon Her with an underabundance of at least 1.5 dex. These underabundances are qualitatively expected from radiative accel eration calculations, which show that Ne has a very small radiative acceler ation in the photosphere, and that it is expected to undergo gravitational settling if the mixing processes are sufficiently weak and there is no stro ng stellar wind. According to theoretical predictions, the low Ne abundance s place an important constraint on the intensity of such stellar winds, whi ch must be less than 10(-14) M-. yr(-1) if they are non-turbulent.