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

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

2000-09-04

arxiv.org/abs/astro-ph/0009047v1

Mon.Not.Roy.Astron.Soc. 318 (2000) 1264

Astronomy and Astrophysics

Astrophysics

10 pages, 1 figure, received 23 June 2000, accepted 4 August 2000, by Monthly Notices of the Royal Astronomical Society

Scientific paper

10.1046/j.1365-8711.2000.03929.x

We make new Non-LTE calculations to deduce abundances of neon from visible-region echelle spectra of selected Ne I lines in 7 normal stars and 20 HgMn stars. We find that the best strong blend-free Ne line which can be used at the lower end of the Teff range is 6402 A, although several other potentially useful Ne I lines are found in the red region of the spectra of these stars. The mean neon abundance in the normal stars (log A =8.10) is in excellent agreement 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 acceleration calculations, which show that Ne has a very small radiative acceleration in the photosphere and is expected to undergo gravitational settling if mixing processes are sufficiently weak, and there is no strong stellar wind. According to the theoretical predictions of Landstreet et al. (1998), the low Ne abundances place an important constraint on the intensity of such stellar winds, which must be less than $10^-14 M_sun per yr if they are non-turbulent.

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