The iron abundance in hot central stars of planetary nebulae derived from IUE spectra
| dc.creator | Deetjen, J. L. | |
| dc.creator | Dreizler, S. | |
| dc.creator | Rauch, T. | |
| dc.creator | Werner, K. | |
| dc.date | 2000-06-23 | |
| dc.date.accessioned | 2026-07-07T01:54:07Z | |
| dc.date.available | 2026-07-07T01:54:07Z | |
| dc.description | We present the first attempt to determine the iron abundance in hot central stars of planetary nebulae. We perform an analysis with fully metal-line blanketed NLTE model atmospheres for a sample of ten stars (T_eff >= 70.000 K) for which high-resolution UV spectra are available from the IUE archive. In all cases lines of Fe VI or Fe VII can be identified. As a general trend, the iron abundance appears to be subsolar by 0.5-1 dex, however, the S/N of the IUE spectra is not sufficient to exclude a solar abundance in any specific case. Improved spectroscopy by either FUSE or HST is necessary to verify the possibility of a general iron deficiency in central stars. The suspected deficiency may be the result of gravitational settling in the case of three high-gravity objects. For the other stars with low gravity and high luminosity dust fractionation during the previous AGB phase is a conceivable origin. | |
| dc.description | 5 pages, 8 figures | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0006338 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0006338 | |
| dc.identifier | Astron. Astrophys. 348, 940-944 (1999) | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/1220 | |
| dc.subject | Astrophysics | |
| dc.title | The iron abundance in hot central stars of planetary nebulae derived from IUE spectra | |
| dc.type | text |