A possible solution to the Lyman/Balmer line problem in hot DA white dwarfs

Preval, S. P. and Barstow, M. A. and Badnell, N. R. and Holberg, J. B. and Hubeny, I.; Dufour, P. and Bergeron, P. and Fontaine, G., eds. (2015) A possible solution to the Lyman/Balmer line problem in hot DA white dwarfs. In: 19th European Workshop on White Dwarfs. Astronomical Society of the Pacific Conference Series, 493 . Astronomical Society of the Pacific, CAN, pp. 15-19. ISBN 9781583818718 (http://aspbooks.org/a/volumes/article_details/?pap...)

[thumbnail of Preval-etal-EWWD2015-Possible-solution-to-the-Lyman-Balmer-line-problem]
Preview
 Text. Filename: Preval_etal_EWWD2015_Possible_solution_to_the_Lyman_Balmer_line_problem.pdf
Accepted Author Manuscript
Download (503kB)| Preview

Abstract

Arguably, the best method for determining the effective temperature (T[subscript: eff]) and surface gravity (log g) of a DA white dwarf is by fitting the Hydrogen Lyman and Balmer absorption features. However, as has been shown for white dwarfs with T[subscript: eff]>50,000K, the calculated value from the Lyman and Balmer lines are discrepant, which worsens with increasing temperature. Many different solutions have been suggested, ranging from the input physics used to calculate the models, to interstellar reddening. We will focus on the former, and consider three variables. The first is the atomic data used, namely the number of transitions included in line blanketing treatments and the photoionization cross sections. The second is the stark broadening treatment used to synthesise the Lyman and Balmer line profiles, namely the calculations performed by Lemke (1997) and Tremblay & Bergeron (2009). Finally, the third is the atmospheric content. The model grids are calculated with a pure H composition, and a metal polluted composition using the abundances of Preval et al. (2013). We present the preliminary results of our analysis, whereby we have determined the T[subscript: eff] for a small selection of white dwarfs. We plan to extend our analysis by allowing metallicity to vary in future model grids.

  • Item type:Book Section
    ID code:58877
    Dates:
    Date
    Event
    30 June 2015
    Published
    Subjects:Science > Astronomy
    Department:Faculty of Science > Physics
    Depositing user: Pure Administrator
    Date deposited:29 Nov 2016 12:54
    Last modified:11 Apr 2024 00:09
    Related URLs:
    URI:https://strathprints.strath.ac.uk/id/eprint/58877
CORE (COnnecting REpositories)