Volume 606, October 2017
|Number of page(s)||27|
|Section||Atomic, molecular, and nuclear data|
|Published online||20 October 2017|
IX. New Se v, Sr iv–vii, Te vi, and I vi oscillator strengths and the Se, Sr, Te, and I abundances in the hot white dwarfs G191−B2B and RE 0503−289⋆,⋆⋆,⋆⋆⋆
1 Institute for Astronomy and Astrophysics, Kepler Center for Astro and Particle Physics, Eberhard Karls University, Sand 1, 72076 Tübingen, Germany
2 Physique Atomique et Astrophysique, Université de Mons, UMONS, 7000 Mons, Belgium
3 IPNAS, Université de Liège, Sart Tilman, 4000 Liège, Belgium
4 NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
5 Astronomisches Rechen-Institut (ARI), Centre for Astronomy of Heidelberg University, Mönchhofstraße 12-14, 69120 Heidelberg, Germany
Received: 2 January 2017
Accepted: 17 June 2017
Context. To analyze spectra of hot stars, advanced non-local thermodynamic equilibrium (NLTE) model-atmosphere techniques are mandatory. Reliable atomic data is crucial for the calculation of such model atmospheres.
Aims. We aim to calculate new Sr iv–vii oscillator strengths to identify for the first time Sr spectral lines in hot white dwarf (WD) stars and to determine the photospheric Sr abundances. To measure the abundances of Se, Te, and I in hot WDs, we aim to compute new Se v, Te vi, and I vi oscillator strengths.
Methods. To consider radiative and collisional bound-bound transitions of Se v, Sr iv - vii, Te vi, and I vi in our NLTE atmosphere models, we calculated oscillator strengths for these ions.
Results. We newly identified four Se v, 23 Sr v, 1 Te vi, and three I vi lines in the ultraviolet (UV) spectrum of RE 0503−289. We measured a photospheric Sr abundance of 6.5+ 3.8-2.4× 10-4 (mass fraction, 9500–23 800 times solar). We determined the abundances of Se (1.6+ 0.9-0.6× 10-3, 8000–20 000), Te (2.5+ 1.5-0.9× 10-4, 11 000–28 000), and I (1.4+ 0.8-0.5× 10-5, 2700–6700). No Se, Sr, Te, and I line was found in the UV spectra of G191−B2B and we could determine only upper abundance limits of approximately 100 times solar.
Conclusions. All identified Se v, Sr v, Te vi, and I vi lines in the UV spectrum of RE 0503−289 were simultaneously well reproduced with our newly calculated oscillator strengths.
Key words: atomic data / line: identification / stars: abundances / stars: individual: G191-B2B / stars: individual: RE 0503-289 / virtual observatory tools
Based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26666.
© ESO, 2017
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