2018A&A...619A.152A


C.D.S. - SIMBAD4 rel 1.7 - 2019.11.18CET00:46:11

2018A&A...619A.152A - Astronomy and Astrophysics, volume 619A, 152-152 (2018/11-1)

Line shapes of the magnesium resonance lines in cool DZ white dwarf atmospheres.

ALLARD N.F., KIELKOPF J.F., BLOUIN S., DUFOUR P., GADEA F.X., LEININGER T. and GUILLON G.

Abstract (from CDS):


Context. Line shapes of the magnesium resonance lines in white dwarf spectra are determined by the properties of magnesium atoms and the structure of the white dwarf atmosphere. Through their blanketing effect, these lines have a dominant influence on the model structure and thus on the determination from the spectra of other physical parameters that describe the stellar atmosphere and elemental abundances.
Aims. In continuation of previous work on Mg+He lines in the UV, we present theoretical profiles of the resonance line of neutral Mg perturbed by He at the extreme density conditions found in the cool largely transparent atmosphere of DZ white dwarfs.
Methods. We accurately determined the broadening of Mg by He in a unified theory of collisional line profiles using ab initio calculations of MgHe potential energies and transition matrix elements among the singlet electronic states that are involved for the observable spectral lines.
Results. We computed the shapes and line parameters of the Mg lines and studied their dependence on helium densities and temperatures. We present results over the full range of temperatures from 4000 to 12000K needed for input to stellar spectra models. Atmosphere models were constructed for a range of effective temperatures and surface gravities typical for cool DZ white dwarfs. We present synthetic spectra tracing the behavior of the Mg resonance line profiles under the low temperatures and high gas pressures prevalent in these atmospheres.
Conclusions. The determination of accurate opacity data of magnesium resonance lines together with an improved atmosphere model code lead to a good fit of cool DZ white dwarf stars. The broadening of spectral lines by helium needs to be understood to accurately determine the H/He and Mg/He abundance ratio in DZ white dwarf atmospheres. We emphasize that no free potential parameters or ad hoc adjustments were used to calculate the line profiles.

Abstract Copyright: © ESO 2018

Journal keyword(s): line: profiles - white dwarfs - line: formation - atomic processes - stars: individual: L 119-34

VizieR on-line data: <Available at CDS (J/A+A/619/A152): fig5.dat>

Simbad objects: 4

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Number of rows : 4

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 EGGR 45 WD* 05 55 09.5304147671 -04 10 07.066181242   15.49 14.45 13.994 13.538 DZ11 104 1
2 LAWD 25 WD* 07 40 20.7887176053 -17 24 49.155097204   13.36 13.061 12.886 12.70 DAZ6 178 0
3 Ross 640 WD* 16 28 25.0030292072 +36 46 15.849157470   14.01   13.9   DZA5.5 161 0
4 LAWD 91 WD* 22 19 48.3087067191 -65 29 17.485183989 13.98 14.66 14.53     DZ5 41 0

    Equat.    Gal    SGal    Ecl

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2019.11.18-00:46:11

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