Hostname: page-component-8448b6f56d-qsmjn Total loading time: 0 Render date: 2024-04-23T22:21:01.505Z Has data issue: false hasContentIssue false
  • English
  • Français

N and Fe-Peak Elemental Abundances from IUE Co-Added Spectra of Hg-Mn and Normal Stars

Published online by Cambridge University Press:  12 April 2016

Scott W. Roby ,
Saul J. Adelman ,
David S. Leckrone ,
Charles Cowley  and
Glenn M. Wahlgren
Scott W. Roby
Affiliation:
Dept. of Phys. and Astr., Univ. of DE, Newark, DE 19716, USA (On leave from Dept. of Earth Sci., SUNY College, Oswego, NY 13126, USA)
Saul J. Adelman
Affiliation:
Dept. of Physics, The Citadel, Charleston, SC 29409, USA
David S. Leckrone
Affiliation:
NASA-Goddard Space Flight Center, Greenbelt, MD 20771, USA
Charles Cowley
Affiliation:
Astronomy Dept., Univ. of Michigan, Ann Arbor, MI 48109, USA
Glenn M. Wahlgren
Affiliation:
CSC/GHRS, Code 680, GSFC, Greenbelt, MD, 20771, USA

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Leckrone and Adelman have established an IUE observing strategy that has yielded co-added spectra with enhanced S/N ratios for several A and B stars. New observations by Roby and Adelman using the same technique have added two new Hg-Mn stars into this sample. We have begun a long-term study of elemental abundances in this uniform, high-quality set of IUE spectra for 13 stars. We report on the first stages of this project: abundances for N, Cr, Mn, Fe, Co, and Ni. The study of the Fe- peak elements show that our data set can provide accurate abundances and that abundances obtained from UV and optical spectra often are in good agreement. This study provides the groundwork for self-consistent abundance analyses of more exotic elements in our long term project.

Type
I. General Properties of CP Stars
Information
International Astronomical Union Colloquium , Volume 138: Peculiar versus Normal Phenomena in A-Type and Related Stars , 1993 , pp. 154 - 160
Copyright
Copyright © Astronomical Society of the Pacific 1993

References

Adelman, S.J. 1988, M.N.R.A.S., 235, 749.Google Scholar
Adelman, S.J. 1989, M.N.R.A.S., 239, 487.Google Scholar
Adelman, S.J. 1991, M.N.R.A.S., 252, 116.Google Scholar
Adelman, S.J. 1992, M.N.R.A.S. in press.Google Scholar
Adelman, S.J., Roby, S.W., Leckrone, D.s., Cowley, C., and Wahlgren, G.M. 1992, in preparation.Google Scholar
Fuhr, J.R., Martin, G.A., and Wiese, W.L. 1988, Journal of Physical and Reference Data, 17, Suppl. 4.Google Scholar
Leckrone, D.S., and Adelman, S.J. 1989, Ap. J. Suppl., 71, 387.CrossRefGoogle Scholar
Kurucz, R.L. 1981, SAO Special Report 390.Google Scholar
Kurucz, R.L. 1992, private communication.Google Scholar
Kurucz, R.L., and Peytremann, E. 1975, SAO Special Report 367.Google Scholar
Martin, G.A., Fuhr, J.R. and Wiese, W.L. 1988, Journal of Physical and Reference Data, 17, Suppl. 3.Google Scholar
Roby, S.W., and Lambert, D.L. 1990, Ap. J. Suppl., 73, 167.Google Scholar
Roby, S.W., Leckrone, D.S., and Adelman, S.J. 1992, in preparation.Google Scholar
Roby, S.W. 1990, in Evolution of Stars: The Photospheric Abundance Connection; Poster Paper Supplement, ed Michaud, G., Tutukov, A., and Bergevin, M., 145th I.A.U. Symposium, p. 75. Google Scholar