Get access

Pressure shifts and abundance gradients in the atmosphere of the DAZ white dwarf GALEX J193156.8+011745

Authors

  • S. Vennes,

    Corresponding author
    1. Astronomickýústav AV ČR, Fričova 298, CZ-251 65 Ondřejov, Czech Republic
    Search for more papers by this author
  • A. Kawka,

    Corresponding author
    1. Astronomickýústav AV ČR, Fričova 298, CZ-251 65 Ondřejov, Czech Republic
    Search for more papers by this author
  • P. Németh

    Corresponding author
    1. Astronomickýústav AV ČR, Fričova 298, CZ-251 65 Ondřejov, Czech Republic
    2. Department of Physics and Space Sciences, 150 W. University Blvd, Florida Institute of Technology, Melbourne, FL 32901, USA
    Search for more papers by this author

  • Based on observations made with European Southern Observatory (ESO) telescopes at the La Silla Paranal Observatory under programme 283.D-5060.

E-mail: vennes@sunstel.asu.cas.cz (SV); kawka@sunstel.asu.cas.cz (AK); nemeth@sunstel.asu.cas.cz (PN)

ABSTRACT

We present a detailed model atmosphere analysis of high-dispersion and high signal-to-noise ratio spectra of the heavily polluted DAZ white dwarf GALEX J1931+0117. The spectra obtained with the Very Large Telescope (VLT)-Kueyen/UV-Visual Echelle Spectrograph show several well-resolved Si ii spectral lines enabling a study of pressure effects on line profiles. We observed large Stark shifts in silicon lines in agreement with theoretical predictions and laboratory measurements. Taking into account Stark shifts in the calculation of synthetic spectra, we reduced the scatter in individual line radial velocity measurements from ∼3 to ≲1 km s−1. We present revised abundances of O, Mg, Si, Ca and Fe based on a critical review of line-broadening parameters and oscillator strengths. The new measurements are generally in agreement with our previous analysis with the exception of magnesium with a revised abundance of a factor of 2 lower than previously estimated. The magnesium, silicon and iron abundances exceed solar abundances, but the oxygen and calcium abundances are below solar. Also, we compared the observed line profiles to synthetic spectra computed with variable accretion rates and vertical abundance distributions assuming diffusive steady state. The inferred accretion rates vary from inline image for calcium to 2 × 109 g s−1 for oxygen. We find that the accretion flow must be oxygen rich while being deficient in calcium relative to solar abundances. The lack of radial velocity variations between two measurement epochs suggests that GALEX J1931+0117 is probably not in a close binary and that the source of the accreted material resides in a debris disc.

Ancillary