Jump to ContentJump to Main Navigation
Show Summary Details
More options …

Open Astronomy

formerly Baltic Astronomy

Editor-in-Chief: Barbuy, Beatriz


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

ICV 2017: 121.03

Open Access
Online
ISSN
2543-6376
See all formats and pricing
More options …
Volume 20, Issue 4

Issues

Stark Broadening and White Dwarfs

Milan S. Dimitrijević
  • Corresponding author
  • Astronomical Observatory, Volgina 7, 11060 Belgrade 38, Serbia France
  • Observatoire de Paris, LERMA, 5 Place Jules Janssen, 92190 Meudon, France
  • Email
  • Other articles by this author:
  • De Gruyter OnlineGoogle Scholar
/ Andjelka Kovačević
  • Department of Astronomy, Faculty of Mathematics, University of Belgrade, Studentski Trg 16, 11000 Belgrade, Serbia
  • Email
  • Other articles by this author:
  • De Gruyter OnlineGoogle Scholar
/ Zoran Simić / Sylvie Sahal-Bréchot
Published Online: 2017-03-23 | DOI: https://doi.org/10.1515/astro-2017-0327

Abstract

White dwarf and pre-white dwarfs are the best types of stars for the application of Stark broadening research results in astrophysics, since in the atmospheres of these stars physical conditions are very favorable for this line broadening mechanism - in hot hydrogen-deficient white dwarfs and pre-white dwarfs Teff = 75 000–180 000 K and log g = 5.5–8 [cgs]. Even for much cooler DA and DB white dwarfs with the typical effective temperatures 10 000-20 000 K, Stark broadening is usually the dominant broadening mechanism. In this review, Stark broadening in white dwarf spectra is considered, and the attention is drawn to the STARK-B database (http://stark-b.obspm.fr/), containing the parameters needed for analysis and synthesis of white dwarf spectra, as well as for the collective efforts to develop the Virtual Atomic and Molecular Data Center.

Keywords: stars; white dwarfs; Stark broadening; line profiles; databases

References

  • Dimitrijević M. S. 2010, Mem. Soc. Astron. Ital., 75, 282Google Scholar

  • Dimitrijević M. S., Dačić M., Cvetković, Z. Simić Z. 2004, A&A, 425, 1147Google Scholar

  • Dimitrijević M. S., Jovanović P., Simić Z. 2003a, A&A, 410, 735Google Scholar

  • Dimitrijević M. S., Ryabchikova T., Popović L. Č.. et al. 2003b, A&A, 404, 1099Google Scholar

  • Dimitrijević M. S., Ryabchikova T., Simić Z. et al. 2007, A&A, 469, 681Google Scholar

  • Dreizler S., Werner K. 1996, A&A, 314, 217Google Scholar

  • Dubernet M. L., Boudon V., Culhane J. L. et al. 2010, JQSRT, 111, 2151Google Scholar

  • Dufour P., Ben Nessib N., Sahal-Bréchot S., Dimitrijević M. S. 2011, Baltic Astronomy, 20, 511 (this issue)Google Scholar

  • Dufour P., Fontaine G., Liebert J. et al. 2008, ApJ, 683, 978Google Scholar

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

  • Fontaine M., Chayer P., Oliveira C. M. et al. 2008, ApJ, 678, 394Google Scholar

  • Hamdi R., Ben Nessib N., Milovanović N. et al. 2008, MNRAS, 387, 871Google Scholar

  • Jevremović D., Dimitrijević M. S., Popović L. Č. et al. 2009, New Astron. Rev., 53, 222Google Scholar

  • Koester D. 2010, Mem. Soc. Astron. Ital., 81, 921Google Scholar

  • Kurucz R. L. 1979, ApJS, 40, 1Google Scholar

  • McGraw J. T., Starrfield S., Liebert J., Green R. F. 1979, in White Dwarfs and Variable Degenerate Stars, IAU Coll. 53, eds. H. M. van Horn & V. Weidemann, Univ. of Rochester, p. 377Google Scholar

  • Milovanović N., Dimitrijević M. S., Popović L. Č., Simić Z. 2004, A&A, 417, 375Google Scholar

  • Nugent J. J., Jensen K. A., Nousek J. A. et al. 1983, ApJS, 51,Google Scholar

  • Popović L.Č., Dimitrijević M. S., Ryabchikova T. 1999a, A&A, 350, 719Google Scholar

  • Popović L.Č., Dimitrijević M. S., Tankosić D. 1999b, A&AS, 139, 617Google Scholar

  • Popović L.Č., Milovanović N., Dimitrijević M. S., 2001a, A&A, 365, 656Google Scholar

  • Popović L.Č., Simić S., Milovanović N., Dimitrijević M. S. 2001b, ApJS, 135, 109Google Scholar

  • Rauch T., Ziegler M., Werner K. et al. 2007, A&A, 470, 317Google Scholar

  • Rixon G., Dubernet M. L., Piskunov N. et al. 2011, AIP Conf. Proc., 1344, 107Google Scholar

  • Simić Z., Dimitrijević M. S., Kovačević A. 2009, New Astron. Rev., 53, 246Google Scholar

  • Simić Z., Dimitrijević M. S., Milovanović N., Sahal-Bréchot S. 2005, A&A, 441, 391Google Scholar

  • Simić Z., Dimitrijević M. S., Popović L. Č., Dačić M. 2006, New Astron., 12, 187Google Scholar

  • Tankosić D., Popović L. Č., Dimitrijević M. S. 2003, A&A, 399, 795Google Scholar

  • Werner K., Heber U., Hunger R. 1991, A&A, 244, 437Google Scholar

  • Werner K., Wolff B. 1999, A&A, 347, L9Google Scholar

  • Wickramasinghe D. T. 1972, Mem. Roy. Astron. Soc., 76, 129Google 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 495–502, ISSN (Online) 2543-6376, DOI: https://doi.org/10.1515/astro-2017-0327.

Export Citation

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

Comments (0)

Please log in or register to comment.
Log in