  Helium-rich subdwarf B (He-sdB) stars represent a small group of low-mass hot
stars with luminosities greater than those of conventional subdwarf B stars,
and effective temperatures lower than those of subdwarf O stars. By measuring
their surface chemistry, we aim to explore the connection between He-sdB stars,
He-rich sdO stars and normal sdB stars. LS IV-14 116 is a relatively
intermediate He-sdB star, also known to be a photometric variable.
High-resolution blue-optical spectroscopy was obtained with the
Anglo-Australian Telescope. Analysis of the spectrum shows LS IV-14 116 to have
effective temperature Teff = 34 000 +/- 500 K, surface gravity log g = 5.6 +/-
0.2, and surface helium abundance nHe = 0.16 +/- 0.03 by number. This places
the star slightly above the standard extended horizontal branch, as represented
by normal sdB stars. The magnesium and silicon abundances indicate the star to
be metal poor relative to the Sun. A number of significant but unfamiliar
absorption lines were identified as being due to germanium, strontium, yttrium
and zirconium. After calculating oscillator strengths (for Ge, Y and Zr), the
photospheric abundances of these elements were established to range from 3 dex
(Ge) to 4 dex (Sr, Y and Zr) above solar. The most likely explanation is that
these overabundances are caused by radiatively-driven diffusion forming a
chemical cloud layer in the photosphere. It is conjectured that this cloud
formation could be mediated by a strong magnetic field.
