In the light of the reported presence by other authors of elements beyond the iron group in the atmospheres of cool DO white dwarfs we search for the presence of these elements across a range of hydrogen deficient stars. We examine a sample of FUSE spectra for the occurrence of these lines and measure their velocity with respect to the stellar velocity in each case. We also ascertain whether or not the lines are photospheric in origin by observing the velocity of the line in two stars of different stellar velocity. Whilst in most cases the identifications of C, N, O, Si, S, and P pass the identity test we find that nearly all of the new proposed identifications fail.
|Title of host publication||Hydrogen-Deficient Stars|
|Publisher||Astronomical Society of the Pacific|
|Number of pages||4|
|Publication status||Published - 2008|
|Name||ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES|
Boyce, D. D., Barstow, M. A., Dobbie, P. D., Aston, J. H., Booles, B. C., Preval, S. P., Laird, R. J. M., James, F. A., Barstow, J. K., & Forbes, A. E. (2008). Post iron group elements in DO stars. In Hydrogen-Deficient Stars (Vol. 391, pp. 235-238). (ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES). Astronomical Society of the Pacific. http://aspbooks.org/custom/publications/paper/391-0235.html