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Open Astronomy

formerly Baltic Astronomy

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IMPACT FACTOR 2017 (Baltic Astronomy): 0.417
5-year IMPACT FACTOR (Baltic Astronomy): 0.486

CiteScore 2017: 0.16

SCImago Journal Rank (SJR) 2017: 0.131
Source Normalized Impact per Paper (SNIP) 2017: 0.109

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ISSN
2543-6376
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Volume 20, Issue 4

Issues

Stark Broadening of Carbon and Oxygen Lines in Hot DQ White Dwarf Stars: Recent Results and Applications

P. Dufour / N. Ben Nessib / S. Sahal-Bréchot / M. S. Dimitrijević
  • Observatoire de Paris, LERMA, CNRS, UMR 8112, 5 Place Jules Janssen, 92190 Meudon, France Serbia
  • Astronomical Observatory, Volgina, 7, 11060 Belgrade 38, Serbia
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Published Online: 2017-03-23 | DOI: https://doi.org/10.1515/astro-2017-0329

Abstract

White dwarf stars are traditionally found to have surface compositions made primarily of hydrogen or helium. However, a new family has recently been uncovered, the so-called hot DQ white dwarfs, which have surface compositions dominated by carbon and oxygen with little or no trace of hydrogen and helium (Dufour et al. 2007, 2008, 2010). Deriving precise atmospheric parameters for these objects (such as the effective temperature and the surface gravity) requires detailed modeling of spectral line profiles. Stark broadening parameters are of crucial importance in that context. We present preliminary results from our new generation of model atmospheres including the latest Stark broadening calculations for C II lines and discuss the implications as well as future work that remains to be done.

Keywords: stars; white dwarfs; fundamental parameters; Stark broadening

References

  • Barlow B. N., Dunlap B. H., Rosen R., Clemens J. C. 2008, ApJ, 688, 95Google Scholar

  • Blagojević B., Popović M. V., Konjević N. 1999, Physica Scripta, 59, 374Google Scholar

  • Castelli F. 2005, Mem. Soc. Astron. Ital. Suppl., 8, 44Google Scholar

  • Djenize S., Srecković A., Milosavljević M., Labat O., Platisa M. 1988, Z. f. Phys. D, 9, 129Google Scholar

  • Dufour P., Liebert J., Fontaine G., Behara N. 2007, Nature, 450, 522Google Scholar

  • Dufour P., Fontaine G., Liebert J., Schmidt G. D., Behara N. 2008, ApJ, 683, 978Google Scholar

  • Dufour P., Liebert J., Swift B. et al. 2009, J. Phys. Conf. Ser., 172, 012012Google Scholar

  • Dufour P., Fontaine G., Bergeron P. et al. 2010, 17th European White Dwarf Workshop, AIP Conf. Proc., 1273, 64Google Scholar

  • Dufour P., Béland S., Fontaine G. et al. 2011, ApJ, 733, 19Google Scholar

  • Dunlap B. H., Barlow B. N., Clemens J. C. 2010, ApJ, 720, 159Google Scholar

  • Goly A., Weniger S. 1982, JQSRT, 28, 389Google Scholar

  • Griem H. R, 1974, Spectral Line Broadening by Plasmas, Academic PressGoogle Scholar

  • Larbi-Terzi N., Sahal-Bréchot S., Ben Nessib N., Dimitrijević M. S. 2010, 17th European White Dwarf Workshop, AIP Conf. Proc., 1273, 428Google Scholar

  • Mahmoudi W. F., Ben Nessib B., Sahal-Bréchot S. 2004, Physica Scripta, 70, 142Google Scholar

  • Montgomery M. H., Williams K. A., winget D. E. et al. 2008, ApJ, 678, 51Google Scholar

  • Peytremann E. 1972, A&A, 17, 76Google Scholar

  • Sahal-Bréchot S. 2010, J. Phys. Conf. Ser., 257, 012028Google Scholar

  • Sahal-Bréchot S., Dimitrijevi´c M. S., Ben Nessib N. 2011, Baltic Astronomy, 20, 523 (this issue)Google Scholar

  • Sahal-Bréchot S., Segre E. R. A. 1971, A&A, 13, 161Google Scholar

  • Sreckovic A., Drincić V., Bukvić S., Djenize S. 2000, J. Phys. B, 33, 4873Google Scholar

About the article

Received: 2011-08-08

Accepted: 2011-08-15

Published Online: 2017-03-23

Published in Print: 2011-12-01


Citation Information: Open Astronomy, Volume 20, Issue 4, Pages 511–515, ISSN (Online) 2543-6376, DOI: https://doi.org/10.1515/astro-2017-0329.

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© 2017. This work is licensed under the Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 License. BY-NC-ND 4.0

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